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The utilization of pulsars as SETI beacons

October 2003
International Journal of Astrobiology 2(4)

DOI:10.1017/S1473550403001666

Authors:

William H. Edmondson

University of Birmingham

I. Stevens

University of Birmingham

This paper proposes that pulsars can serve as beacons for the discovery of and communication with extraterrestrials. The motivation for the communication strategy proposed is discussed in detail, along with relevant astrophysical considerations. It is shown that millisecond pulsars have characteristics and a distribution in space that make it possible to envisage communication being targeted towards and away from habstars (as defined by Turnbull & Tarter) aligned with pulsars in a specified way. Lists of candidate habstars and their pulsar alignments are included for those wishing to conduct searches using the strategy described.

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The utilization of pulsars as SETI beacons

William H. Edmondson

and Ian R. Stevens

School of Computer Science,University of Birmingham,Birmingham B15 2TT,UK

e-mail: w.h.edmondson@cs.bham.ac.uk

School of Physics and Astronomy,University of Birmingham,Birmingham B15 2TT,UK

e-mail: irs@star.sr.bham.ac.uk

Abstract: This paper proposes that pulsars can serve as beacons for the discovery of and

communication with extraterrestrials. The motivation for the communication strategy proposed is

discussed in detail, along with relevant astrophysical considerations. It is shown that millisecond pulsars

have characteristics and a distribution in space that make it possible to envisage communication being

targeted towards and away from habstars (as deﬁned by Turnbull & Tarter) aligned with pulsars in a

speciﬁed way. Lists of candidate habstars and their pulsar alignments are included for those wishing to

conduct searches using the strategy described.

Received 30 September 2003, accepted 30 October 2003

Key words: beacons, pulsars, SETI.

Introduction

SETI paradigms apparently fall into simple categories :

(1) general surveys versus directed searches and

(2) those motivated by zero, weak or strong communicative

intention.

It is possible to discuss options within such a schematic

framework in terms of a focus which is either primarily on the

properties and characteristics of signals that might be em-

ployed, or on the strategy of the enterprise, as presumed to be

adopted by both Earthlings and extraterrestrial intelligences

(ETIs). Our stance is to focus on the strategic issues for dis-

covery, and work toward commentary on signalling charac-

teristics. This stance contrasts with an alternative approach

sometimes found in the SETI community, where it is assumed

that discovery is bound up with signalling characteristics and

content, so that discovery might depend upon successfully

working out what an ETI might try to communicate, and how

(cf. Cordes & Sullivan 1995). Consequently we do not con-

cern ourselves with message design and content.

Various assumptions underpin the current strategies that

diﬀer in terms of resource implications and the interpret-

ations placed upon null results. This paper does not attempt a

comprehensive review or evaluation of the various assump-

tions and plausibilities of these approaches, or of the searches

actually being done, although we do locate some existing

eﬀorts within the scheme outlined above. Rather, our con-

cern is to propose and justify a new paradigm. The proposal

here takes further the ideas proposed earlier by one of us

(Edmondson 2003).

Within the scheme outlined above the new proposal can be

classiﬁed as a directed search with strong communicative

intent. The novelty of the proposal is the use of pulsars

as beacons in relation to communicative intent. We ﬁrst

consider the motivation for the proposal, then the relevant

astrophysical factors and ﬁnally we look at the merits.

It should be noted that the proposal given here is not the

same as that discussed by Heidmann (1988), who was not

concerned with the use of pulsars as directional beacons.

Corbet (1999) has proposed that gamma-ray bursts should be

used as both directional and time markers in SETI strategies.

Some of the issues noted by Corbet are relevant to our pro-

posal and these are touched on below.

Communicative intent

The motivation for the new proposal arises out of consider-

ation of communicative intent. In humans communicative

intent is as important as content. For SETI to be successful,

we argue, it is necessary to develop an approach to this par-

ticular communication situation that reﬂects understanding

of the cognitive and intentional context within which com-

munication operates generally. In relation to the SETI en-

terprise we consider that communicative intent can be zero,

weak or strong.

Zero intent

This term applies to the situation where we Earthlings have

very little communicative intent (but enough to conduct a

search). Furthermore, we assume that the ETIs we look for

do not have communicative intent. The only mechanism for

search that is open to us in this situation is to try to eavesdrop

on ETIs, on the assumption that the ETIs concerned do not

intend their interplanetary radar, or local TV transmissions,

or whatever, to be of interest to another intelligence. This

approach is problematic because (1) the radio frequencies at

which to search are diﬃcult to determine and (2) the power

levels at the transmitter may be relatively low. Plausibly the

International Journal of Astrobiology 2 (4): 231–271 (2003) Printed in the United Kingdom

DOI: 10.1017/S1473550403001666 f2003 Cambridge University Press

231

most promising signal to listen for here would be the use of

radar for interplanetary science, but the problem of identify-

ing candidate frequencies will be compounded by the fact

that such transmissions will be unpredictably infrequent and

intermittent. It is widely assumed in the SETI community

that low transmitter power levels do not present an insur-

mountable obstacle to discovery (trade-oﬀs are possible in

relation to signal processing, antenna gain, frequency, and so

forth, and receiver technology is good). For our purposes

here it is not relevant to explore these issues further as the

zero-intent model is undirected and unintentional and thus

antithetical to the new paradigm.

Weak intent

Current terrestrial SETI activity has weak communicative

intent. Attempts to transmit signals

express weak intent

because they are little more than shots in the dark.

General survey searches for signals (perhaps continuous wave

transmission at 1420 MHz – see http://seti1.setileague.org/

articles/protectd.htm for a list of possible frequencies, and

Blair (1995) for a discussion of possible frequencies) from

ETIs are not directed and presume only some eventual com-

municative intent on our part. Discussions of diﬀerent sig-

nalling paradigms (see Shostak 1995) do not really address

the issue of intentionality.

Considerable eﬀorts are being made in this style of SETI

activity. For example, the resource implications of the

SETI enterprise based in Berkeley are impressive. For several

decades a professional academic resource has been devoted

to devising and implementing techniques for ETI signal

acquisition (including use of Arecibo facilities) and process-

ing (the SETI@Home software is a signiﬁcant demonstration

of the power of grid computing). Indeed, it is arguable that

this sustained level of work is what currently motivates

popular interest in the topic as well as professional concerns

to ﬁnd new paradigms.

Note, however, that all this work should not mask

assumptions about our intent or that of the putative ETIs. It

is not the case that we Earthlings are spending much time

analysing the approaches we should take to begin trans-

missions ourselves (this is distinct from message design). We

assume that ETIs will not have complex strategies, or that if

they do then we will be in the pool of those likely to be

recipients of messages. On this basis the currently null

result can be interpreted variously as bad luck, inadequate

technology, insuﬃcient time, lack of inventiveness in re-

lation to signalling options, etc. Additionally, the recent

production of a list of 17 129 nearby stars with characteristics

appropriate for habitable planets (habstars, see Turnbull &

Tarter 2003a) provides only another opportunity to direct

the search at possible/likely sources without altering as-

sumptions concerning what to search for or why any ETI is

transmitting anything anyway. The assumption is that ETIs

are trying to get in touch with other ETIs – somehow – and

that we can beneﬁt from this without actually making the

eﬀort to join in.

Strong intent

To consider strong communicative intent we need to look at

some challenging questions. For example, what does it mean

to attribute communicative intent to an ETI ? How might we

recognize such an intent ? What must we say about our in-

tention and its expression ? How do these issues inform or

motivate a search for ETIs ? These questions might be sum-

marized as follows: if Earthlings established a designed and

systematic programme to begin long-term continuous trans-

missions in an eﬀort to establish contact with an ETI, what

would this look like?

With regard to strong intentionality we can say the

following.

(1) Any system needs to be based on the assumption that we,

as much as an ETI, want to be successful in establishing

contact.

(2) We know that both an ETI and ourselves share the same

problems.

(3) We must presume that both an ETI and ourselves share

the same solutions.

(4) We and ETIs should expect to target transmissions

according to a predictable and thus shared procedure.

(5) We need to be close to the point of pressing the send

button if we are to be conﬁdent of our search strategy.

(6) We want to be sure of a clear positive or negative outcome.

Consider that on the part of an ETI, weak intentionality

amounts to little more than ‘shouting ’ in the hope that

somewhere someone will ‘hear ’. This is communicative of

little more than existence, in a certain direction (and perhaps

only within a certain volume of the galaxy if a habstar is not

identiﬁed). As the basis for the start of an interaction it is

woefully inadequate, not least because it ignores the possi-

bility that more can be done to establish the initial contact in

ways that might subsequently be useful. The concern here is

not about message composition; the issue rather is that

the presumed intent of an ETI could be a useful basis for

constraining a search and thus improving the chances of

success. However, the ETI has to make the right decisions.

Even in the case of a targeted search directed at habstars,

intentionality could remain weak if an ETI was relatively

thoughtless about the problems facing those seeking to

establish contact.

Strong intentionality can be assumed of an ETI who goes

about the business of transmitting a signal with an intent to

maximize the chances of discovery and the utility of that

discovery in relation to subsequent activity. Work in cogni-

tive science, on distributed cognition (see Hutchins 1996),

encourages us to assume that both an ETI and ourselves have

the same problem to solve and that we will both be concerned

to ﬁnd a recoverably shared solution to a known shared

problem. One way to understand this is to assume that we

Earthlings should ask ourselves ‘ how would we maximize

our discoverability by an ETI? ’ One answer, we propose, is

that we should direct continuous transmissions in speciﬁed

See, e.g., http://www.reuters.com/newsArticle.jhtml?type=science-

News&storyID=3039848&fromEmail=true

W.H. Edmondson and I.R. Stevens232

directions, and with signals speciﬁed in such a way as to be

readily recoverable. Correspondingly, our search should be

targeted in terms of both direction and signal character-

istics – using the same speciﬁcations. The assumption that

the speciﬁcation of the transmission/search paradigm can be

shared, and that this enhances the prospects for success

and subsequent communication, is what distinguishes the

proposal here from those that have been made before.

Corbet (1999) assumed a similar line of reasoning as that

above, although not explicitly formulated in relation to intent

and distributed cognition. Corbet’s concern was to maximize

eﬃciency by means of brief directed transmissions (con-

trasted with continuous omni-directional transmissions),

although he recognized the need for transmitter and receiver

to share understanding of the technique he proposed. The

problematic nature of his proposal is that it is opportunisti-

cally dependent on cosmological events, and that the signal

characteristics are not speciﬁed. The proposal here is to use

pulsars as beacons, thus providing the basis for continuous

signalling. Additionally, pulsars oﬀer a speciﬁcation of the

signal characteristic being sent/sought. Both proposals are

concerned to specify direction of transmission, and in a

similar way, but the additional detail of our proposal is that

transmissions are targeted at candidate stars selected as

putative habitable systems (Turnbull & Tarter 2003a).

Beacons

The speciﬁcations we propose are simple.

(1) The hydrogen line frequency is likely to be ubiquitously

recognized (it is not parochially salient) and so can form

the basis for any signal (this is uncontentious in the sense

that many searches are conducted on this assumption

already).

(2) Signal characteristics can be speciﬁed in detail by the pul-

sar characteristics chosen for beacons, i.e. the signal can

be pulsed at the repetition rates of the pulsars concerned.

(3) No correction is needed for pulse rate or base frequency

modulation caused by the orbital motion of the ETI (this

is richly informative and must be known by any ETI to

be so).

(4) Directions can be speciﬁed in relation to pulsars acting as

beacons – both transmissions and searches are aligned

with the beacons.

(5) Transmissions can be targeted at identiﬁed habstars, and

potential habstar sources can be identiﬁed (Turnbull &

Tarter 2003a).

The core concept underlying the scheme is that an ETI will

align their transmission in relation to a pulsar as a beacon.

This alignment was originally envisaged as being, in a general

sense, ‘anti-pulsar ’ so that an ETI broadcasting a signal will

do so ‘toward the pulsar ’ used to determine its property –

that is, ‘toward the beacon ’ (see, e.g., Corbet 1999 ; cf.

Edmondson 2003). Terrestrial scientists, sharing and thus

knowing ETI’s strategy, need only look ‘ away from ’ pulsars

for speciﬁable signals at the pulse rate of the speciﬁed pulsar.

Such a signal is maximally artefactual in an astrophysical

sense (i.e. very unlikely to be considered a natural phenom-

enon), and this signals recoverable intent.

Directional beacons

The details of the scheme need a little ﬁne tuning – the sense

of ‘toward the beacon ’ needs to be reﬁned to cover habstars

within a reasonable (arbitrary) angular distance of the bea-

con. Rather than inject huge energies into a transmission

antenna with low gain (large beam width) it makes sense to

pick the identiﬁable habstars within a speciﬁed angular range

and to target those with high-gain antennae. That is what we

Earthlings would do if we were concerned to maximize our

discoverability. So, in reciprocal fashion, we should look in

‘anti-pulsar ’ directions (similarly reﬁned in deﬁnition) for

signals at 1420 MHz and with pulse rates speciﬁed by the

pulsars ‘behind us ’ when we turn our antennae towards the

identiﬁed habstars. The assumption is that ETIs will have/

share a concept of habstars (otherwise why would they bother

transmitting anything at all?) and will have identiﬁed a list

closely aligned to ours. The assumptions in relation to identi-

fying habstars are addressed later.

The original supposition was that the search in anti-pulsar

directions is preferentially motivated over all other directions

because any signal found will be maximally artefactual. This

strengthens the sense of shared solution – shared between

ourselves and an ETI – and thus ﬂags the search as being

highly motivated because the underlying assumption is that

the communicative intent of the ETI is strong and unam-

biguous. This line of reasoning has an intuitive appeal to it ;

the proposal is rather ‘obvious ’. However, we need to recall

that the resolution of the antennae involved is such that

searching will not be generally ‘anti-pulsar ’ but will be di-

rected to speciﬁc habstars within any given angular notion of

‘anti-pulsar ’. Likewise, we must assume that ETIs will be

directing their signals at habstars (such as our own) suf-

ﬁciently closely aligned with the ‘ toward pulsar’ direction – as

explained above – but precisely speciﬁed in terms of direction

so as to be aligned with the pulsars but not directed exactly

towards them. This observation allows us to generalize the

notion of demonstrating artefactuality by basing the para-

digm on directional alignment with pulsar beacons rather

than on one speciﬁc direction. It follows from this that we

could also be directing our search in the ‘ toward pulsar ’ di-

rection (reﬁned as above), and our attempts at transmission

in the ‘anti-pulsar ’ direction (reﬁned as above). Jean Schnei-

der (personal communication) made the suggestion that

searching could be ‘toward pulsar’ as much as ‘ anti-pulsar ’

and we acknowledge that elaboration.

Identifying beacons

The issue of which pulsars to use as beacons is interesting.

Consideration of pulsar properties (Lorimer 2001; Hobbs &

Manchester 2003; Manchester et al. 2003) shows that a small

sub-group of pulsars, commonly referred to as ‘millisecond ’

pulsars, have pulse periods of y1–20 ms and that these pul-

sars are remarkably stable. Fast pulsars are attractive because

Utilization of pulsars 233

if the pulse rate is to form the basis of any coding system then

the bit rate will be correspondingly fast (in comparison to the

much more numerous ‘normal ’ pulsars with pulse periods of

a second or more). The fact that some of these pulsars

are found in globular star clusters, and thus overlap when

deployed as directional beacons, is unfortunate in that it

diminishes the spread of coverage of the sky. However, the

millisecond pulsars are more isotropically distributed in the

sky than normal pulsars (Lorimer 2001), which means that

alignment with habstars is likely to be more readily found.

This is illustrated in Fig. 1.

Habstars

The Turnbull & Tarter (2003a) habstar catalogue (HabCat)

is used here to identify targets appropriately aligned with

pulsars. This is discussed below. We should note ﬁrst, how-

ever, that the habstar list is produced with a bias toward

terrestrial life-forms. Such stars are considered potential suns

for ‘habitable ’ planets that are likely to be suﬃciently like

Earth to have life-forms suﬃciently like our own. Note,

however, that a life-form based on radically diﬀerent bio-

physics and biochemistry may have evolved to the point

of producing its own habstar catalogue covering a rather

diﬀerent set of stars. This is perhaps far-fetched, but the point

here is simply that if we can develop a habstar list, and an ETI

somewhere produces a similar list, then shared biophysics and

biochemistry are much more probable.

Our paradigm requires a list of habstars aligned with

pulsars. Working with the original preference we focus ﬁrst

here on the list of habstars that are ‘anti-pulsar ’ in direction.

We then extend the scheme to cover those aligned in the

direction of pulsars. In both cases the notion of alignment

needs an angular deﬁnition, which we consider below, but

further than this there are some technical issues to be clariﬁed

in terms of possibilities and problems, and it is to these we

turn next.

Astrophysical considerations

The properties and distributions of pulsars are helpfully

summarized in the database available online from the

Australian Telescope National Facility (ATNF) (Hobbs &

Manchester 2003; see also Manchester et al. 2003). The

habstar list (Turnbull & Tarter 2003a) is also available online.

Lorimer (2001) provides a comprehensive summary of pulsar

physics. Fig. 2 shows the distribution of pulsars from Hobbs

& Manchester’s list of 1300 pulsars; the plot is of log pulsar

period against log pulsar period derivative, adjusted to bring

the zero on the yaxis into alignment with the millisecond

group to highlight the diﬀerences between these pulsars and

the normal group. Visual inspection leads to identiﬁcation of

an intermediate group which may be closely aligned with the

so-called ‘intermediate-mass binary pulsars ’ (see Lorimer

2001) and which lies between the millisecond pulsars and

Spatial distribution

–100

–80

–60

–40

–20

100

0 6 12 18 24

Dec

millisecond

intermediate

normal

sinusoidal model

clusters

Fig. 1. This shows the spatial distribution of pulsars from the catalogue produced by Hobbs & Manchester (2003). A simple density

modulated sinusoidal model is imposed on the data to guide the reader regarding the galactic distribution of objects. The locations of star

clusters associated with pulsars are also shown. Pulsars for which no value is given for pulse period derivative are not shown (the data

plotted here are those used in the Fig. 2, which requires a value for the derivative).

W.H. Edmondson and I.R. Stevens234

those that are normal. The boundaries between the three

classes are not clear.

Pulsars and habstars

The discoverability of pulsars appears to be determined by

the eﬀort made to ﬁnd them, but in relation to presupposi-

tions made about any ETI’s knowledge of pulsars this issue

needs to be considered in detail. From a terrestrial perspective

there seems to be an entirely unremarkable drift to ﬁnd pul-

sars that are a bit weaker, further or faster, but nonetheless

there are no dramatic trends in the data concerning either

pulse period or location or power, as a function of discovery

date (see Fig. 3 – data from Hobbs & Manchester 2003). It

does appear from the depiction of the data that faster pulsars

have been discovered more recently, but the trend is not

disconcerting. It could be argued that discovery of pulsars,

especially the fast ones, is so recent in astronomical terms

that we are not able to assume much of an ETI’s knowledge

of this class of objects. Against this must be set the argument

that if our set of known pulsars is technology limited (and an

ETI has better technology) then increased receiver sensitivity

will be known by the ETI to be an issue and they will pref-

erentially select the more powerful pulsars for use as bea-

cons. Additionally, of course, greater receiver sensitivity is

probably more likely to increase the distance at which known

pulsars are located than it is to increase the number of known

pulsars at currently common distances. The implication is

that the pulsar density is in fact already known fairly well,

and that better technology will simple sample more of the

galaxy. However, this increase in the pulsar inventory would

be aligned more with the galactic plane and this would not

greatly enhance the sampling of the HabCat.

We might reasonably assume, therefore, that if an ETI

orbiting a habstar knows about pulsars then they know about

a set of objects in space that matches more or less the set

we know about, without systematic diﬀerences from our set.

Note that the SETI paradigm proposed here is not limited to

any speciﬁc pulsar population – as they are discovered so they

can be included in the SETI strategy discussed here. Clearly,

the larger the set the more likely that this set matches well the

set known by an ETI, and that the beacon selection and

alignment will be suited for our detection of that ETI. This

factor contributes to the complexity of the sampling which is

inherent in the proposed paradigm (see below).

Pulsar pulse rates are curiously distributed – as shown in

Fig. 2 – and Lorimer discusses the evolutionary model that

accounts for this. It should be noted that the comparable

ﬁgure in Lorimer’s paper is based on fewer data. We have

chosen, somewhat arbitrarily, to limit the list for initial use to

those with periods of 16 ms or less. As discussed above, faster

Period by derivative

–4

–2

5- 2.5 - 2 -1. 0.5 0 0.5 1 1.5

Log10 period

Log10 period in seconds derivative magnitude, adjusted by 1019

millisecond

intermediate

normal

Fig. 2. This shows the distribution of pulsars organized by period and stability. The axes are logarithmic, and the X-axis shows period with

the Y-axis showing stability (magnitude of the derivative of the period). Three groups of pulsars are identiﬁed – millisecond, intermediate,

normal, with the groupings being determined visually. The boundary between the millisecond and the intermediate groups is at that period

above which a normal pulsar might be found (where normal is independently identiﬁed by the rate of change of period associated with the

normal group in the literature). On the graph above this point is identiﬁable by the fastest outlier of the normal group. The distinction

between intermediate and normal is made subjectively.

Utilization of pulsars 235

pulsars are to be preferred. It is assumed that any such dis-

tribution mapped by an ETI will look similar and that they

will make similar decisions about inclusion in the population

of beacons. Note, it makes sense for both parties to start

work with the shortest period pulsars, and to prefer to work

with short periods whenever possible.

Pulsars are noted for having signiﬁcant proper motion

in space. Inspection of the ﬁgures shows that they are suf-

ﬁciently distant from us (in comparison with the much closer

habstars) that the directions speciﬁed as beacons do not

move signiﬁcantly in relation to the identiﬁcation of habstars

as targets. Fast pulsars have slower proper motion (Lorimer

2001 quotes ﬁgures of y450 km s

for normal pulsars

and y80–140 km s

for millisecond pulsars). Because of

ﬁnite light travel time and stellar proper motions, the level

of alignment between habstars and pulsars will alter

with time.

For the purposes of this paper the relevant timescale is

the light travel time from the Earth to a potential habstar

(and back). If in this timescale the pulsars or habstars were

to move a signiﬁcant distance on the sky then this would

degrade the use of a beacon. As noted by Turnbull & Tarter

(2003a) the typical habstar is y100 pc distant from us and

thus the travel timescale (return trip) will be of the order of

650 yr. If we assume that the proper motion of the habstars

with respect to the Sun is of the order of 50 km s

(Turnbull

& Tarter 2003a), then this motion corresponds to an apparent

motion on the sky of much less than 1x(for an assumed

distance of 100 pc). Indeed for a habstar to move an apparent

distance of 1xon the sky in 650 yr and at a distance of 100 pc

would correspond to a velocity in the plane of the sky much

greater than the escape velocity of the Galaxy. Although

normal pulsars typically have a larger proper motion due to

the kick resulting from the originating supernova, because

they are typically further away once again the apparent

motion on the sky will be small.

The millisecond pulsars and habstars have similar apparent

distributions on the sky (but note that the normal pulsars

are more concentrated in the galactic plane, cf. Fig. 1). For

the habstars, the peak in the distribution of distances is at

around 100 pc (Turnbull & Tarter 2003a). The largest dis-

tance included in the catalogue is 300 pc. This distance range

and limit means that the habstars are distributed roughly

isotropically on the sky, the scale height of main sequence

stars in the Galaxy being of the order of 300 pc (Gilmore &

Reid 1983). An issue with the distribution of pulsars is the

concentration of them in globular clusters (see also Fig. 1)

such as M15 and 47 Tucanae, where in the latter case there

are at least 20 ms pulsars alone (Freire et al. 2003). These

concentrations of millisecond pulsars all within a degree of

each other will naturally lead to multiple tie-ups between

habstars, where one habstar is within the corresponding cone

of a number of pulsars (it was noted earlier that such multiple

tie-ups were unfortunate ; the upside is that this distribution

date effects

–4

–3

–2

–1

1965 1970 1975 1980 1985 1990 1995 2000 2005

‘Discovery date’

Log various values for distance, power, period

distance

power

period

Poly. (distance)

Poly. (power)

Poly. (period)

Fig. 3. This sketch shows the discovery date eﬀects listing in Hobbs & Manchester (2003) arranged as a function of logarithmic values of

distance, power and period, with polynomial loose ﬁts to the data. The trends are unexceptional – indeed they seem intuitively predictable.

The notable feature is the discovery of faster pulsars since the early 1980s, but there is no indication that we are moving to a phase of

discovery of markedly diﬀerent stellar objects. The date values are adjusted for the data sets to avoid overlapping of symbols in the sketch.

W.H. Edmondson and I.R. Stevens236

may serve usefully as the basis for multichannel communi-

cation sharing, to a signiﬁcant extent, a direction).

Identiﬁcation of target beacons and habstars

The current catalogue populations of habstars (17 129) and

pulsars (1300) are signiﬁcantly diﬀerent. The subset of fast

pulsars to be considered for use as beacons is rather small.

The list of habstars has to be processed to ﬁnd alignments

with the selected pulsars – and in this regard Schneider’s

elaboration is useful because it will eﬀectively double the set

of potential target habstars.

It is worth commenting on the projected density of the

habstars on the sky. Isotropic distribution on the sky would

correspond to 0.4 habstar deg

. A consequence of this is

that choosing a random point on the sky and searching with a

radius of 1xwill result in typically around one habstar being

detected within this region. Although arbitrary this seems to

us a sensible initial value to use in computing pulsar–habstar

alignments.

In order to focus the search for beacons (deﬁned by

pulsar–habstar alignment) we concentrate on ‘ millisecond ’

pulsars. These are shown in Fig. 2 as the lower left-hand

group. The group is roughly deﬁned by the limits P

spin

16 ms and |dP/dt|<2r10

(there is a millisecond pulsar

with P

spin

=16.052 (J2145x0750), and another with |dP/dt|

=2.03r10

). This obviously reduces very substantially the

number of pulsars – from 1300 in the basic pulsar catalogue

down to 73 (75 including the two just outside the limits). As

mentioned above, choosing a search radius of 1xaround the

positions and anti-positions of these pulsars will mean that

on average there will be around one habstar in this zone. It

should be noted that several pulsars do not have a measured

value listed for dP/dtand these are not included in the

calculations here (they are included in the full listing in the

Appendix, with the dP/dtvalue set to 1).

In order to search for useful positional correspondence

between pulsars and habstars, so as to deﬁne a useful set of

beacons, we adopt the following criteria. Based on the

position of each pulsar, we calculate the pulsar anti-position

on the sky and then deﬁne a search cone of radius 1xaround

this pulsar anti-position (deﬁned as the location on the sky

that is diametrically opposite the position of the pulsar). We

then determine whether there is a habstar within this search

radius. We repeat the procedure for the pulsar position. The

ﬁrst procedure is based on the proposed ETI beaming a signal

towards the pulsar beacons and the second on the ETI

beaming a signal directly away from any such pulsar beacon.

Tables 1 and 2 present lists of habstars that are aligned

‘anti-pulsar ’ and ‘ toward pulsar ’, in relation to the milli-

second pulsars identiﬁed above. In connection with Table 1

we note that the total number of correlations is 53 ; the

number of diﬀerent pulsars in this sample is 30 ; the number

of diﬀerent habstars is 52. There are three habstars with

two pulsars in this sample, and a few pulsars with more

than one habstar. (If J2145x0750 is included the numbers

increase to 56, 31, 55, because it anti-aligns with three

habstars.)

In connection with Table 2 we note that the total number

of correlations is 60; the number of diﬀerent pulsars in this

sample is 44; the number of diﬀerent habstars is 45. In this

sample there is one habstar (index number 2186) that is in the

same direction as 15 pulsars. The star is called HD2466 and it

just happens to be near to the 47 Tucanae globular cluster

(and so has lots of pulsars within 1x). It is not in the cluster

(which is much further away), there is just a chance super-

position.

The data in Tables 1 and 2 show that pulsar alignments do

sample the habstar population with suﬃcient density to yield

useful lists – 97 habstars aligned with 55 fast pulsars is a good

starting point for experimental work to explore the possibility

that pulsars can serve as beacons (note that there are 19

pulsars common to Tables 1 and 2).

It is sensible here to recall that the identiﬁcation of group-

ings in the pulsar population is rather subjective. It turns out,

for example, that the fast outlier normal pulsar (see Fig. 2),

J0537x6910, could easily serve as a beacon (well oﬀ the

galactic plane, reasonably fast with P

spin

=16.115 ms). It

happens not to match any habstars with our alignment

criteria so does not appear in the listings. This point is taken

up later.

Signal characteristics

The assumption that an ETI will transmit at the period

speciﬁed by the pulsar to which the transmission is aligned

facilitates discovery and could provide a rich source of data

about an ETI’s planetary system. The known periodicity

makes signal recovery from noise easier because summation

of data over the suspected period can be used (cf. the use

of this technique to recover details of pulsar pulse shape,

Lorimer 2001). Additionally, the use of a single transmission

frequency (say 1420 MHz) dispenses with the need to con-

sider dispersion corrections. Certainly, there are other aspects

of signalling design that need to be resolved (e.g. to combat

fading/scintillation) but these can be tackled after discovery,

not as part of reﬁnement of discovery procedures. It can be

assumed that an ETI will maintain a constant pulse period

(derivable even when the pulsar is part of a binary system)

with suﬃcient accuracy that their own motion will be recov-

erable from perturbations in period. Indeed, it may be poss-

ible to disentangle several details of an ETI’s environment:

spin about the axis of their own planet, orbital details, plan-

etary system details (and thus these characteristics do not

have to be encoded in the message – cf. Sullivan & Cordes

1995).

As noted by Corbet (1999) the energy required to transmit

a continuous signal can be used to produce a more powerful

(detectable) signal if the transmission is pulsed – ‘providing

the recipient knows where and when a signal is coming from ’.

In our scheme the pulse rate determines much of what the

recipient needs to know for signal detection, and the mark/

space ratio will also help if short, perhaps 1 : 10 (roughly

typical of pulsars; although there is no need to mimic the

beacon’s pulse characteristics). The directional aspect of

the search is sorted out by the alignments as discussed

Utilization of pulsars 237

Table 1. A list of potential beacons for ETI searches. Listed are positional coincidences (within 1x)between pulsar anti-positions

on the sky and stars in the habstar list of Turnbull & Tarter (2003a). Shown in this table are the pulsar name,pulsar period and

period derivative,pulsar position (in J2000 coordinates), and for the corresponding habstar,the Hipparcos ID number and the

position are shown (in J2000 coordinates)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J0034x0534 0.00188 0.496Ex20 8.5908 x5.5768 61 261 188.3188 5.7815 0.3405

J0034x0534 0.00188 0.496Ex20 8.5908 x5.5768 61 341 188.5329 4.9616 0.6180

J0218+4232 0.00232 0.774Ex19 34.5262 42.5382 69 795 214.2679 x42.8625 0.4146

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 81101 248.4792 47.2716 0.8365

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 81242 248.8888 47.6831 0.6063

J0613x0200 0.00306 0.957Ex20 93.4329 x2.0131 89 207 273.0754 1.8975 0.3757

J0613x0200 0.00306 0.957Ex20 93.4329 x2.0131 89 412 273.6892 1.7584 0.3613

J0751+1807 0.00348 0.778Ex20 117.7879 18.1274 97 596 297.5579 x17.9539 0.2881

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 333 332.2475 x52.7688 0.9574

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 787 333.5763 x53.2999 0.4737

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 956 334.0387 x53.5529 0.9995

J1024x0719 0.00516 0.185Ex19 156.1612 x7.3219 110760 336.5812 7.9036 0.7174

J1024x0719 0.00516 0.185Ex19 156.1612 x7.3219 110782 336.6504 6.5504 0.9135

J1045x4509 0.00747 0.177Ex19 161.4588 x45.1650 112 379 341.4146 45.3897 0.2290

B1257+12 0.00622 0.114Ex18 195.0125 12.6824 4699 15.0942 x13.5992 0.9204

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 15 256 49.1958 x2.5839 0.6600

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 15 500 49.9346 x2.0715 0.3042

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 15 256 49.1958 x2.5839 0.6627

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 15 500 49.9346 x2.0715 0.2965

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 21 918 70.7029 12.2103 0.2912

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 22 012 70.9729 12.6858 0.2770

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 22 021 71.0154 12.9912 0.5847

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 291 75.1533 29.4729 0.6526

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 302 75.1750 30.8972 0.7990

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 438 75.5733 29.9950 0.2940

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 291 75.1533 29.4729 0.6609

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 302 75.1750 30.8972 0.7911

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 438 75.5733 29.9950 0.2961

J1713+0747 0.00457 0.854Ex20 258.4563 7.7937 24 353 78.3862 x7.3299 0.4691

J1713+0747 0.00457 0.854Ex20 258.4563 7.7937 24 472 78.7825 x7.3458 0.5542

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 25 586 82.0250 22.9307 0.5832

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 25 652 82.1992 23.9581 0.9653

J1732x5049 0.00531 0.138Ex19 263.1988 x50.8167 26 113 83.5362 51.2162 0.5230

J1740x5340 0.00365 0.168Ex18 265.1854 x53.6780 26 871 85.5804 53.5156 0.4271

J1740x5340 0.00365 0.168Ex18 265.1854 x53.6780 26 933 85.7446 54.2576 0.8054

B1744x24A 0.01156 x0.340Ex19 267.0092 x24.7769 27236 86.5846 25.4764 0.8183

B1744x24A 0.01156 x0.340Ex19 267.0092 x24.7769 27640 87.7604 25.2288 0.8767

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 28 528 90.3258 27.2816 0.7622

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 29 074 91.9958 27.4284 0.9181

B1855+09 0.00536 0.178Ex19 284.4013 9.7215 33 109 103.4367 x9.5154 0.9864

J1910x5959A 0.00327 0.307Ex20 287.9279 x59.9741 34 804 108.0712 59.2652 0.7233

J1910x5959C 0.00528 0.220Ex20 287.7729 x60.0166 34 804 108.0712 59.2652 0.8085

J1911x1114 0.00363 0.142Ex19 287.9550 x11.2395 34 767 107.9629 10.5122 0.7274

B1937+21 0.00156 0.105Ex18 294.9104 21.5831 37 217 114.6692 x21.2234 0.4331

J2033+17 0.00595 0.110Ex19 308.3375 17.6000 42 281 129.3150 x17.4948 0.9832

J2051x0827 0.00451 0.127Ex19 312.7812 x8.4605 43 618 133.2563 9.1858 0.8670

J2051x0827 0.00451 0.127Ex19 312.7812 x8.4605 43 692 133.4908 8.4215 0.7106

J2124x3358 0.00493 0.205Ex19 321.1825 x33.9789 46 022 140.7904 33.9056 0.3989

J2124x3358 0.00493 0.205Ex19 321.1825 x33.9789 46 098 141.0100 34.7969 0.8359

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 297 157.1775 x27.3654 0.6936

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 494 157.7537 x26.8675 0.3217

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 657 158.3067 x26.8142 0.8489

J2317+1439 0.00344 0.242Ex20 349.2883 14.6587 55 066 169.0925 x14.6931 0.1988

W.H. Edmondson and I.R. Stevens238

Table 2. A list of potential beacons for ETI searches. Listed are positional coincidences (within 1x)between pulsar positions on

the sky and stars in the habstar list of Turnbull & Tarter (2003a). Shown in this table are the pulsar name,pulsar period and

period derivative,pulsar position (in J2000 coordinates), and for the corresponding habstar,the Hipparcos ID number and the

position are shown (in J2000 coordinates)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B0021x72C 0.00576 x0.499Ex19 5.9596 x72.0754 2186 6.9092 x71.8826 0.9689

B0021x72D 0.00536 x0.343Ex20 6.0575 x72.0788 2186 6.9092 x71.8826 0.8740

B0021x72E 0.00354 0.985Ex19 6.0462 x72.0889 2186 6.9092 x71.8826 0.8872

B0021x72F 0.00262 0.645Ex19 6.0158 x72.0786 2186 6.9092 x71.8826 0.9146

B0021x72G 0.00404 x0.421Ex19 6.0329 x72.0777 2186 6.9092 x71.8826 0.8977

B0021x72H 0.00321 x0.184Ex20 6.0279 x72.0685 2186 6.9092 x71.8826 0.9006

B0021x72I 0.00348 x0.459Ex19 6.0329 x72.0777 2186 6.9092 x71.8826 0.8977

B0021x72J 0.00210 x0.979Ex20 5.9975 x72.0663 2186 6.9092 x71.8826 0.9300

B0021x72L 0.00435 x0.122Ex18 6.0154 x72.0825 2186 6.9092 x71.8826 0.9158

B0021x72M 0.00368 x0.384Ex19 5.9767 x72.0919 1779 5.6446 x73.0323 0.9973

B0021x72M 0.00368 x0.384Ex19 5.9767 x72.0919 2186 6.9092 x71.8826 0.9557

B0021x72N 0.00305 x0.219Ex19 6.0379 x72.0747 2186 6.9092 x71.8826 0.8922

J0024x7204O 0.00264 0.304Ex19 6.0192 x72.0816 2186 6.9092 x71.8826 0.9120

J0024x7204Q 0.00403 0.340Ex19 6.0683 x72.0736 2186 6.9092 x71.8826 0.8623

J0024x7204S 0.00283 x0.121Ex18 6.0163 x72.0784 2186 6.9092 x71.8826 0.9141

J0024x7204U 0.00434 0.952Ex19 6.0408 x72.0666 2186 6.9092 x71.8826 0.8876

J0030+0451 0.00487 0.100Ex19 7.6142 4.8610 2659 8.4200 4.9478 0.8105

J0034x0534 0.00188 0.496Ex20 8.5908 x5.5768 2980 9.4867 x5.9979 0.9899

J0218+4232 0.00232 0.774Ex19 34.5262 42.5382 10 753 34.5808 41.9297 0.6109

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 21 425 69.0008 x47.6551 0.5111

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 21 458 69.1108 x46.4855 0.7937

J0711x6830 0.00549 0.149Ex19 107.9758 x68.5132 34 805 108.0721 x67.7823 0.7372

J0711x6830 0.00549 0.149Ex19 107.9758 x68.5132 35 052 108.7346 x68.0708 0.8783

J1045x4509 0.00747 0.177Ex19 161.4588 x45.1650 52 629 161.4388 x45.7589 0.5942

J1045x4509 0.00747 0.177Ex19 161.4588 x45.1650 52 666 161.5379 x45.7904 0.6304

B1257+12 0.00622 0.114Ex18 195.0125 12.6824 63 577 195.4238 13.1736 0.6406

J1455x3330 0.00799 0.243Ex19 223.9496 x33.5129 72 761 223.1212 x33.2672 0.8640

J1455x3330 0.00799 0.243Ex19 223.9496 x33.5129 72 991 223.7429 x34.4454 0.9552

J1455x3330 0.00799 0.243Ex19 223.9496 x33.5129 73 140 224.2038 x34.2465 0.7764

J1455x3330 0.00799 0.243Ex19 223.9496 x33.5129 73 221 224.4650 x33.2740 0.5681

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 74 907 229.6304 1.7697 0.3179

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 75 222 230.5779 2.0069 0.9505

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 74 907 229.6304 1.7697 0.3213

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 75 222 230.5779 2.0069 0.9429

J1629x6902 0.00600 0.100Ex19 247.2863 x69.0459 80 733 247.2388 x68.4179 0.6297

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 83 241 255.1913 x30.5162 0.4226

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 83 522 256.0404 x30.6593 0.9212

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 83 241 255.1913 x30.5162 0.4151

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 83 522 256.0404 x30.6593 0.9154

J1713+0747 0.00457 0.854Ex20 258.4563 7.7937 84 521 259.1713 8.0586 0.7625

J1721x2457 0.00350 0.590Ex20 260.2725 x24.9517 84 907 260.2812 x24.6835 0.2683

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 85 561 262.2779 x23.8359 0.8221

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 85 642 262.5271 x22.9513 0.1391

J1740x5340 0.00365 0.168Ex18 265.1854 x53.6780 86 347 264.6679 x54.4694 0.9455

J1744x1134 0.00408 0.894Ex20 266.1221 x11.5818 86 702 265.7284 x10.7948 0.8800

J1757x5322 0.00887 0.263Ex19 269.3129 x53.3740 87 793 269.0179 x53.5824 0.3613

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 88 354 270.6383 x27.7796 0.6632

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 88 465 270.9533 x26.8398 0.4718

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 88 683 271.5571 x27.4926 0.5102

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 88 746 271.7567 x27.1020 0.6952

J1910x5959A 0.00327 0.307Ex20 287.9279 x59.9741 94 410 288.2263 x59.6888 0.4128

J1910x5959C 0.00528 0.220Ex20 287.7729 x60.0166 94 410 288.2263 x59.6888 0.5594

J1911x1114 0.00363 0.142Ex19 287.9550 x11.2395 94 017 287.1234 x11.1856 0.8334

B1937+21 0.00156 0.105Ex18 294.9104 21.5831 96 912 295.5025 22.2827 0.9166

B1953+29 0.00613 0.297Ex19 298.8658 29.1454 98 151 299.2021 29.5309 0.5115

B1953+29 0.00613 0.297Ex19 298.8658 29.1454 98 185 299.2938 29.9269 0.8910

J2129x5721 0.00373 0.207Ex19 322.3446 x57.3539 105 838 321.5550 x57.9499 0.9894

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 110 946 337.1808 26.7257 0.2809

J2317+1439 0.00344 0.242Ex20 349.2883 14.6587 114 739 348.6388 15.2118 0.8531

J2322+2057 0.00481 0.970Ex20 350.5929 20.9508 115 417 350.7017 20.5590 0.4066

Utilization of pulsars 239

earlier and tabulated in Tables 1 and 2. A null, to a given

signal strength, is readily determined and can be listed in a

catalogue, either for a repeat assessment or for the develop-

ment of more sophisticated receiver systems if technological

limits are thought relevant. A target habstar in this scheme

can be investigated with <100 min of data (thousands of

pulse periods overlaid for initial scrutiny), permitting

straightforward data acquisition and archiving for oﬄine

processing. Plausibly, simple summation of signals over the

pulse period will suﬃce for initial assessment as minor devi-

ations in period (due to ETI’s orbital motion, or whatever)

can be recovered subsequently.

Power levels appropriate for signal detection of an ETI

using a directional signal are discussed by Turnbull & Tarter

(2003a) in relation to the distribution of distances in their

HabCat. They note that ‘the farthest star in the HabCat

is at y300 pc, and transmitted powers comparable to the

Arecibo planetary radar will be detectable to the ATA

[Allen Telescope Array] at this distance ’. Habstar motion

implies the need to use a transmission beamwidth of several

arcmin, such as might be achieved with a 100 m dish at

1420 MHz. Signals are thus likely to be on the borderline

of detectability without additional techniques such as sum-

mation.

The discussion here is concerned with SETI rather than

with the details of what an ETI might be trying to com-

municate. Additionally, by focusing on SETI we also mean

to de-emphasize the more complex issues of designing a

systematic communications protocol – the two topics are

not the same. Following the discovery of an ETI using a

beacon it then becomes possible to consider what solutions

might be shared in relation to multiple channels, fading,

etc.

Conclusion

The paradigm sketched above is simple to comprehend and

exploit, suitable for repeated measures, extremely sensitive

and ultimately rather obvious in relation to the desire to es-

tablish recognizable artefactuality in the solution to a known

shared problem. A null result for any pulsar alignment is

probably unequivocal (at the time of assessment) and not

technology limited. The main drawback is that the scheme

really only samples the sky.

The cynical astronomer might argue that the proposal is

rather like looking for one’s lost key under the street-

lamp – because that is where the light is. The reality is diﬀer-

ent: the proposal identiﬁes a reason for looking in a speciﬁc

direction, at speciﬁc targets, for speciﬁc signals with pulse

rates such that data rates for a transmission are usefully high.

The use of the HabCat signiﬁcantly enhances the value of the

scheme, but it remains the case that the sample covered is still

less than 1% of the habstar population (using millisecond

pulsars).

As noted earlier, the pulsar groupings are arbitrary as

well as the criteria, and they are really mentioned only in

order to provide a convenient way of referring to the faster

and more stable subset of the total pulsar population. The

initial criteria (P

spin

<16 ms, |dP/dt|<2r10

) could be

relaxed to include some intermediate pulsars and fast

normal pulsars, especially if they do not lie in the galactic

plane (J0537x6910 provides a good example). This would

enlarge the potential for ﬁnding pulsar–habstar alignments.

Another way of doing this is to retain the criteria and enlarge

the habstar listing. We have learned (Maggie Turnbull,

personal communication) that a more extensive HabCat is

forthcoming (Turnbull & Tarter 2003b), and although many

of the objects in the new list lie at considerable distances

from us (mean distance of 240 pc) the list will usefully aug-

ment the opportunities for ﬁnding pulsar–habstar alignments

as described here.

The list of candidate alignments could be enlarged mark-

edly by using all pulsars, regardless of pulsar stability and

pulse rate. The coverage is substantially higher – 1858

habstars, which is approximately 10 % of the habstar popu-

lation (see the Appendix). The disadvantage of doing this,

from an ETI’s point of view as much as ours, is that the

transmission rate could be very slow. The compensation,

for any ETI as much as ourselves, is that such a scheme

for transmission will not use a huge amount of energy as the

transmission pulses will mostly be interleaved. Communica-

tions protocols and message content, should we decide to

transmit, or should we detect anything, are other issues

entirely and will be covered in a separate publication.

One potentially serious objection to the proposed scheme

is that ETIs sending pulses might be thought to be detectable

as pulsar-like objects. These have not already been detected

and surely this ‘null result ’ must make the scheme implaus-

ible. In fact the proposal permits manageable energies to be

put into signalling for discoverability using the paradigm,

without having to broadcast infeasible energies in general

mimicry of pulsars (for which the established discovery pro-

cedure is diﬀerent), or more broadly for detection by SETI

programmes. In short, the current pulsar discovery techni-

ques are really unlikely to have turned up any ETI transmit-

ting on one or a few frequencies at a speciﬁc pulse rate,

and SETI searches more generally will fail if they look

for suﬃciently energetic continuous wave transmissions

rather than pulsed transmissions. Signal overlay techniques

using data from a known direction, at a presumed frequency,

and with predicted pulse rate, permit a possible signal to be

dredged out of noise levels that are otherwise likely to

be intractable (permitting feasibly low transmitter power

for an ETI community to establish and resource a scheme

for broadcasting).

One practical way of countering the objection is simply to

check the habstars identiﬁed in the tables given in the paper

and the Appendix. It is to be expected that even the amateur

radio astronomy community might have the resources to

check the habstars listed. It is our view that the scheme is

plausible, worthwhile and practical – null results should be

quickly and inexpensively available. Positive results would

be interesting.

W.H. Edmondson and I.R. Stevens240

Appendix

Tables A1 and A2 provide the full sets of correlations in anti-pulsar (792) and pulsar (1066) alignments as described for the

millisecond pulsars in the body of the paper.

Table A1. 792 c orrelations between pulsar anti-positions and the habstar catalogue

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J0006+1834 0.69375 0.210Ex14 1.5200 18.5831 58 900 181.1883 x17.8510 0.8037

J0006+1834 0.69375 0.210Ex14 1.5200 18.5831 59 089 181.7596 x19.5303 0.9771

B0011+47 1.24070 0.564Ex15 3.5738 47.7759 59 693 183.6192 x47.6128 0.1694

J0034x0534 0.00188 0.496Ex20 8.5908 x5.5768 61 261 188.3188 5.7815 0.3405

J0034x0534 0.00188 0.496Ex20 8.5908 x5.5768 61 341 188.5329 4.9616 0.6180

B0031x07 0.94295 0.408Ex15 8.5367 x7.3648 61 419 188.7825 7.4429 0.2579

B0031x07 0.94295 0.408Ex15 8.5367 x7.3648 61 561 189.2033 7.9332 0.8761

B0037+56 1.11822 0.288Ex14 10.1346 57.2736 61 716 189.7550 x56.9106 0.5252

B0037+56 1.11822 0.288Ex14 10.1346 57.2736 61 744 189.8154 x57.3235 0.3230

B0037+56 1.11822 0.288Ex14 10.1346 57.2736 61 928 190.3708 x56.3046 0.9974

J0051+0423 0.35473 0.700Ex17 12.8754 4.3803 62 898 193.3600 x5.0036 0.7896

J0051+0423 0.35473 0.700Ex17 12.8754 4.3803 63 070 193.8413 x4.5043 0.9738

B0052+51 2.11517 0.954Ex14 13.9388 51.2902 63 224 194.3204 x52.0491 0.8494

B0053+47 0.47204 0.333Ex14 14.1063 47.9363 62 903 193.3825 x47.8884 0.7253

B0053+47 0.47204 0.333Ex14 14.1063 47.9363 62 955 193.5029 x48.5818 0.8836

B0053+47 0.47204 0.333Ex14 14.1063 47.9363 63 229 194.3400 x48.6360 0.7377

J0100x7211 5.43987 0.150Ex10 15.1796 x72.1927 63 614 195.5650 72.4852 0.4839

B0059+65 1.67916 0.595Ex14 15.6371 65.6204 63 797 196.1292 x65.9217 0.5770

B0105+65 1.28366 0.131Ex13 17.0942 66.1428 63 797 196.1292 x65.9217 0.9900

B0105+65 1.28366 0.131Ex13 17.0942 66.1428 63 906 196.4442 x66.3509 0.6825

B0105+68 1.07112 0.481Ex16 17.1229 69.0979 63 925 196.4983 x68.5717 0.8167

J0108x1431 0.80756 0.770Ex16 17.0346 x14.5303 63 923 196.4967 14.8395 0.6204

J0108x1431 0.80756 0.770Ex16 17.0346 x14.5303 63 976 196.6496 15.3739 0.9273

J0108x1431 0.80756 0.770Ex16 17.0346 x14.5303 64 254 197.5508 15.3383 0.9589

J0108x1431 0.80756 0.770Ex16 17.0346 x14.5303 64 344 197.8404 14.3286 0.8307

B0114+58 0.10144 0.585Ex14 19.4108 59.2440 65 058 200.0337 x59.4410 0.6533

J0133x6957 0.46347 0.120Ex15 23.3850 x69.9582 66 388 204.1742 69.7766 0.8098

J0134x2937 0.13696 0.784Ex16 23.5775 x29.6213 65 985 202.9354 29.7987 0.6661

J0134x2937 0.13696 0.784Ex16 23.5775 x29.6213 66 244 203.6604 28.8359 0.7898

J0134x2937 0.13696 0.784Ex16 23.5775 x29.6213 66 277 203.7592 30.1445 0.5538

J0137+16 0.41477 0.100E+01 24.3792 16.9167 66 203 203.5446 x16.3889 0.9874

J0137+16 0.41477 0.100E+01 24.3792 16.9167 66 231 203.6087 x17.3511 0.8845

J0137+16 0.41477 0.100E+01 24.3792 16.9167 66 319 203.8792 x16.9239 0.5001

B0136+57 0.27245 0.107Ex13 24.8321 58.2421 66 632 204.8671 x57.2970 0.9458

B0136+57 0.27245 0.107Ex13 24.8321 58.2421 66 793 205.3454 x57.4479 0.9457

B0138+59 1.22295 0.391Ex15 25.4163 60.1590 66 557 204.6517 x59.8422 0.8276

B0138+59 1.22295 0.391Ex15 25.4163 60.1590 66 676 205.0317 x60.5567 0.5533

B0138+59 1.22295 0.391Ex15 25.4163 60.1590 66 693 205.0700 x60.2660 0.3624

B0138+59 1.22295 0.391Ex15 25.4163 60.1590 66 752 205.2271 x60.5988 0.4788

B0149x16 0.83274 0.130Ex14 28.0450 x16.6314 67 580 207.7146 16.2546 0.5012

J0205+6449 0.06569 0.194Ex12 31.4079 64.8286 68 804 211.2925 x64.3528 0.4895

J0205+6449 0.06569 0.194Ex12 31.4079 64.8286 68 869 211.5413 x65.7241 0.9055

B0203x40 0.63055 0.120Ex14 31.5050 x40.4679 68 745 211.0775 40.3502 0.4434

B0203x40 0.63055 0.120Ex14 31.5050 x40.4679 68 963 211.7708 40.7681 0.4010

J0218+4232 0.00232 0.774Ex19 34.5262 42.5382 69 795 214.2679 x42.8625 0.4146

B0226+70 1.46682 0.311Ex14 37.8083 70.4427 70 872 217.4004 x70.7919 0.5369

J0248+60 0.21700 0.100E+01 42.0000 60.0000 72 490 222.3354 x60.0797 0.3447

B0320+39 3.03207 0.636Ex15 50.8608 39.7481 75 490 231.3121 x39.3348 0.6119

J0329+16 0.89330 0.100E+01 52.3042 16.9000 75 798 232.2804 x17.3818 0.4824

B0353+52 0.19703 0.477Ex15 59.4367 52.6160 77 944 238.7583 x53.1377 0.8557

B0402+61 0.59457 0.558Ex14 61.6250 61.6447 78 674 240.9192 x61.4709 0.7269

J0417+35 0.65440 0.100E+01 64.4292 35.7500 79 884 244.5879 x36.5660 0.8313

J0417+35 0.65440 0.100E+01 64.4292 35.7500 80 025 245.0363 x36.2876 0.8109

J0421x0345 2.16131 0.116Ex14 65.3896 x3.7519 79 991 244.9350 2.9013 0.9645

J0435+27 0.32628 0.100E+01 68.8917 27.7333 81 456 249.5583 x27.0363 0.9645

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 81 101 248.4792 47.2716 0.8365

J0437x4715 0.00576 0.573Ex19 69.3154 x47.2523 81 242 248.8888 47.6831 0.6063

Utilization of pulsars 241

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J0448x2749 0.45045 0.148Ex15 72.1729 x27.8296 82 354 252.4092 28.3418 0.5640

J0448x2749 0.45045 0.148Ex15 72.1729 x27.8296 82 359 252.4333 28.3851 0.6135

B0450x18 0.54894 0.575Ex14 73.1417 x17.9898 82 568 253.1713 18.0622 0.0782

B0450x18 0.54894 0.575Ex14 73.1417 x17.9898 82 712 253.6029 18.7435 0.8836

B0450+55 0.34073 0.237Ex14 73.5321 55.7282 82 490 252.8862 x55.2999 0.7750

B0456x69 0.32042 0.102Ex13 73.9479 x69.8595 82 887 254.0791 69.0087 0.8609

J0459x0210 1.13308 0.140Ex14 74.9663 x2.1685 83 027 254.5017 2.3419 0.4959

B0458+46 0.63857 0.558Ex14 75.5187 46.9017 83 122 254.7967 x46.9504 0.7237

B0458+46 0.63857 0.558Ex14 75.5187 46.9017 83 381 255.6237 x46.5849 0.3337

B0458+46 0.63857 0.558Ex14 75.5187 46.9017 83 460 255.8696 x46.4542 0.5686

B0525+21 3.74551 0.400Ex13 82.2179 22.0003 85 285 261.4025 x21.6317 0.8949

B0525+21 3.74551 0.400Ex13 82.2179 22.0003 85 642 262.5271 x22.9513 1.0000

B0531+21 0.03308 0.423Ex12 83.6329 22.0144 85 908 263.3354 x21.3045 0.7697

J0538+2817 0.14316 0.367Ex14 84.6042 28.2859 86 376 264.7529 x28.4124 0.1953

B0540x69 0.05035 0.479Ex12 85.0467 x69.3319 86 775 265.9825 69.0741 0.9707

J0540x7125 1.28602 0.820Ex15 85.1283 x71.4254 86 568 265.3637 70.4642 0.9896

J0540x7125 1.28602 0.820Ex15 85.1283 x71.4254 86 804 266.0638 71.1973 0.9628

J0611+30 1.41209 0.100E+01 92.8167 30.2667 89 036 272.5871 x31.1119 0.8759

J0613x0200 0.00306 0.957Ex20 93.4329 x2.0131 89 207 273.0754 1.8975 0.3757

J0613x0200 0.00306 0.957Ex20 93.4329 x2.0131 89 412 273.6892 1.7584 0.3613

B0626+24 0.47662 0.200Ex14 97.2737 24.2616 90 523 277.0713 x23.5687 0.7218

B0626+24 0.47662 0.200Ex14 97.2737 24.2616 90 574 277.2363 x25.0428 0.7822

B0626+24 0.47662 0.200Ex14 97.2737 24.2616 90 861 278.0325 x24.7331 0.8934

J0633+1746 0.23709 0.110Ex13 98.4750 17.7699 90 788 277.8279 x17.7820 0.6472

B0656+14 0.38489 0.550Ex13 104.9504 14.2393 93 398 285.3312 x13.6906 0.6679

J0711+0931 1.21409 0.400Ex15 107.9004 9.5236 94 516 288.5504 x9.9709 0.7890

J0725x1635 0.42431 0.926Ex16 111.2517 x16.5961 95 598 291.6612 16.0024 0.7212

B0727x18 0.51016 0.190Ex13 112.3846 x18.6119 95 721 292.0500 18.9175 0.4531

B0727x18 0.51016 0.190Ex13 112.3846 x18.6119 96 037 292.9075 17.7832 0.9798

J0737x2202 0.32037 0.547Ex14 114.4333 x22.0348 96 447 294.1296 22.6005 0.6421

B0736x40 0.37492 0.162Ex14 114.6346 x40.7112 96 528 294.3654 40.5889 0.2956

B0740x28 0.16676 0.168Ex13 115.7042 x28.3788 97 012 295.7600 27.9433 0.4390

B0743x53 0.21484 0.273Ex14 116.2596 x53.8561 97 286 296.5800 54.6385 0.8455

J0751+1807 0.00348 0.778Ex20 117.7879 18.1274 97 596 297.5579 x17.9539 0.2881

B0751+32 1.44235 0.108Ex14 118.6692 32.5323 97 927 298.5237 x32.0031 0.5488

B0751+32 1.44235 0.108Ex14 118.6692 32.5323 97 977 298.6800 x33.2871 0.7549

B0823+26 0.53066 0.171Ex14 126.7137 26.6233 100 883 306.8329 x27.4456 0.8309

B0823+26 0.53066 0.171Ex14 126.7137 26.6233 101 003 307.1613 x26.2640 0.5739

J0834x4159 0.12112 0.444Ex14 128.5679 x41.9975 101 763 309.3737 42.5543 0.9795

J0835x3707 0.54140 0.978Ex14 128.7625 x37.1310 101 614 308.9109 36.4754 0.6721

B0835x41 0.75162 0.354Ex14 129.3379 x41.5873 101 763 309.3737 42.5543 0.9677

B0835x41 0.75162 0.354Ex14 129.3379 x41.5873 101 989 310.0321 41.2528 0.7706

B0841+80 1.60223 0.446Ex15 132.2563 80.4831 102 742 312.2784 x81.1701 0.6874

B0853x33 1.26754 0.632Ex14 133.9100 x33.5276 102 985 312.9825 33.2782 0.9605

B0853x33 1.26754 0.632Ex14 133.9100 x33.5276 103 232 313.7075 32.7063 0.8459

J0855x4644 0.06469 0.726Ex14 133.9004 x46.7371 103 523 314.6038 46.6040 0.7158

J0855x4658 0.57507 0.136Ex13 133.8313 x46.9729 103 523 314.6038 46.6040 0.8561

B0855x61 0.96251 0.168Ex14 134.2471 x61.6315 103 394 314.2108 61.5608 0.0794

B0855x61 0.96251 0.168Ex14 134.2471 x61.6315 103 614 314.8946 61.2818 0.7359

J0857x4424 0.32677 0.233Ex13 134.4796 x44.4029 103 694 315.1854 44.7853 0.8028

J0901x4624 0.44199 0.875Ex13 135.4171 x46.4135 103 523 314.6038 46.6040 0.8353

B0903x42 0.96517 0.189Ex14 136.2467 x42.7706 104 369 317.1591 42.5356 0.9423

J0905x4536 0.98828 0.149Ex15 136.3496 x45.6147 104 407 317.2671 45.9868 0.9901

J0905x5127 0.34629 0.249Ex13 136.4662 x51.4635 104 084 316.3087 51.1510 0.3500

B0905x51 0.25356 0.183Ex14 136.8163 x51.9664 104 084 316.3087 51.1510 0.9605

B0906x17 0.40163 0.669Ex15 137.1587 x17.6604 104 333 317.0221 17.1073 0.5698

B0909x71 1.36289 0.333Ex15 137.4000 x72.2023 104 682 318.0725 72.4716 0.7244

B0917+63 1.56799 0.361Ex14 140.3088 62.9039 105 276 319.8542 x62.1528 0.8779

J0922x4949 0.95029 0.976Ex13 140.5621 x49.8200 105 290 319.9000 49.2212 0.8927

J0927+23 0.76189 0.100E+01 141.9042 23.7833 105 740 321.2571 x23.3185 0.7967

J0927+23 0.76189 0.100E+01 141.9042 23.7833 105 789 321.3696 x23.5811 0.5716

J0927+23 0.76189 0.100E+01 141.9042 23.7833 106 204 322.6767 x24.1683 0.8631

J0932x3217 1.93163 0.250Ex15 143.1629 x32.2873 106 473 323.4758 32.8694 0.6609

W.H. Edmondson and I.R. Stevens242

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B0932x52 1.44477 0.464Ex14 143.6179 x52.8242 106 794 324.4579 53.0801 0.8781

J0943+22 0.53291 0.100E+01 145.8542 22.9333 107 052 325.2225 x22.7816 0.6496

B0942x13 0.57026 0.453Ex16 146.1204 x13.9116 107 494 326.5808 14.6322 0.8551

J0945x4833 0.33159 0.483Ex14 146.4092 x48.5540 107 713 327.2992 48.4373 0.8976

B0943+10 1.09771 0.349Ex14 146.5317 9.8653 107 266 325.8971 x9.9934 0.6474

J0947+27 0.85105 0.100E+01 146.8417 27.7000 107 305 326.0062 x27.8933 0.8575

J0947+27 0.85105 0.100E+01 146.8417 27.7000 107 817 327.6375 x27.3366 0.8749

B0950x38 1.37381 0.580Ex15 148.0717 x38.6528 108 014 328.2450 38.3434 0.3546

B0950x38 1.37381 0.580Ex15 148.0717 x38.6528 108 154 328.6808 38.2356 0.7384

B0950x38 1.37381 0.580Ex15 148.0717 x38.6528 108 231 328.8912 38.8166 0.8358

B0959x54 1.43658 0.514Ex13 150.4079 x55.1185 108 689 330.2646 55.9987 0.8917

B0959x54 1.43658 0.514Ex13 150.4079 x55.1185 108 921 330.9500 55.8491 0.9097

J1001x5559 1.66118 0.860Ex15 150.2858 x55.9834 108 689 330.2646 55.9987 0.0262

J1001x5559 1.66118 0.860Ex15 150.2858 x55.9834 108 921 330.9500 55.8491 0.6776

J1002x5559 0.77750 0.157Ex14 150.7413 x55.9936 108 689 330.2646 55.9987 0.4767

J1002x5559 0.77750 0.157Ex14 150.7413 x55.9936 108 921 330.9500 55.8491 0.2539

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 333 332.2475 x52.7688 0.9574

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 787 333.5763 x53.2999 0.4737

J1012+5307 0.00526 0.171Ex19 153.1392 53.1174 109 956 334.0387 x53.5529 0.9995

J1012x5830 2.13359 0.377Ex13 153.2287 x58.5071 109 425 332.5433 57.8222 0.9690

J1012x5830 2.13359 0.377Ex13 153.2287 x58.5071 109 841 333.6988 57.7107 0.9248

J1015x5719 0.13988 0.574Ex13 153.9079 x57.3202 109 767 333.5038 57.1200 0.4510

J1015x5719 0.13988 0.574Ex13 153.9079 x57.3202 109 841 333.6988 57.7107 0.4430

J1015x5719 0.13988 0.574Ex13 153.9079 x57.3202 110 056 334.3675 58.0855 0.8927

J1016x5819 0.08783 0.698Ex15 154.0504 x58.3170 109 841 333.6988 57.7107 0.7009

J1016x5819 0.08783 0.698Ex15 154.0504 x58.3170 110 056 334.3675 58.0855 0.3926

J1016x5857 0.10738 0.806Ex13 154.0879 x58.9534 110 056 334.3675 58.0855 0.9118

B1015x56 0.50346 0.313Ex14 154.3033 x56.3585 110 327 335.1904 56.1139 0.9202

B1016x16 1.80470 0.174Ex14 154.6679 x16.7028 109 950 334.0246 16.0209 0.9375

J1019x5749 0.16250 0.201Ex13 154.9671 x57.8183 110 056 334.3675 58.0855 0.6564

J1024x0719 0.00516 0.185Ex19 156.1612 x7.3219 110 760 336.5812 7.9036 0.7174

J1024x0719 0.00516 0.185Ex19 156.1612 x7.3219 110 782 336.6504 6.5504 0.9135

J1035x6345 0.57958 0.350Ex15 158.7625 x63.7551 111 496 338.8383 64.3814 0.6309

J1045x4509 0.00747 0.177Ex19 161.4588 x45.1650 112 379 341.4146 45.3897 0.2290

B1055x52 0.19711 0.583Ex14 164.4950 x52.4490 113 202 343.8646 52.6221 0.6538

B1056x57 1.18500 0.430Ex14 164.7538 x57.7039 113 755 345.5533 58.2547 0.9709

B1112+50 1.65644 0.249Ex14 168.9100 50.5034 114 950 349.2433 x51.3191 0.8812

J1117x6447 1.15527 0.240Ex15 169.4375 x64.7994 114 792 348.8021 65.0123 0.6701

B1119x54 0.53578 0.277Ex14 170.3296 x54.7349 115 222 350.0738 54.4874 0.3559

J1123x4844 0.24484 0.654Ex16 170.8150 x48.7396 115 282 350.2258 48.1129 0.8602

J1126x6942 0.57942 0.330Ex14 171.5900 x69.7042 115 604 351.2733 69.9499 0.4007

J1130x5826 0.16232 0.159Ex16 172.5679 x58.4340 116 085 352.8371 59.1653 0.7792

J1130x5925 0.68098 0.952Ex15 172.5433 x59.4261 116 085 352.8371 59.1653 0.3929

B1131x62 1.02287 0.452Ex15 173.4642 x62.8474 116 221 353.2225 63.1554 0.3915

B1133+16 1.18791 0.373Ex14 174.0129 15.8527 116 590 354.4088 x15.2146 0.7509

B1133x55 0.36471 0.822Ex14 174.0088 x55.4190 116 497 354.1046 55.4957 0.1227

J1141x3107 0.53843 0.196Ex14 175.3567 x31.1313 116 744 354.8996 30.9988 0.4759

J1141x3322 0.29147 0.463Ex15 175.4279 x33.3771 117 059 355.9617 32.5465 0.9873

J1152x6012 0.37657 0.669Ex14 178.2242 x60.2058 117 795 358.3321 59.9450 0.2822

J1210x5209 0.42413 0.200Ex13 182.5021 x52.4419 894 2.7421 52.4428 0.2400

J1215x5328 0.63641 0.115Ex15 183.7525 x53.4754 1224 3.8104 53.0741 0.4055

J1216x6223 0.37405 0.168Ex13 184.1742 x62.3994 1184 3.6988 62.1964 0.5170

J1220x6318 0.78921 0.800Ex16 185.0742 x63.3129 1673 5.2333 63.6675 0.3887

J1224x6208 0.58576 0.202Ex13 186.1842 x62.1448 1846 5.8338 61.2155 0.9931

B1221x63 0.21648 0.495Ex14 186.0921 x64.1316 1673 5.2333 63.6675 0.9761

J1225x6035 0.62632 0.288Ex15 186.3692 x60.5938 1846 5.8338 61.2155 0.8205

J1225x6035 0.62632 0.288Ex15 186.3692 x60.5938 2131 6.7575 60.4025 0.4329

J1231x47 1.87320 0.100E+01 187.9167 x47.7667 2712 8.6221 47.9154 0.7209

J1231x6303 1.35124 0.140Ex14 187.8042 x63.0550 2717 8.6475 62.5905 0.9628

J1233x6312 0.56476 0.692Ex14 188.3813 x63.2081 2717 8.6475 62.5905 0.6725

J1236x5033 0.29476 0.156Ex15 189.2462 x50.5601 2602 8.2633 50.4930 0.9852

J1238+21 1.11859 0.145Ex14 189.5962 21.8697 3003 9.5487 x22.2638 0.3970

J1238+21 1.11859 0.145Ex14 189.5962 21.8697 3024 9.6321 x21.2842 0.5866

Utilization of pulsars 243

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J1238+21 1.11859 0.145Ex14 189.5962 21.8697 3051 9.6887 x21.0401 0.8348

B1237+25 1.38245 0.960Ex15 189.9179 24.8972 2902 9.1950 x24.5008 0.8245

B1237+25 1.38245 0.960Ex15 189.9179 24.8972 3099 9.8612 x24.5235 0.3780

B1237x41 0.51224 0.174Ex14 190.0733 x41.4144 3293 10.5058 40.6884 0.8450

B1237x41 0.51224 0.174Ex14 190.0733 x41.4144 3333 10.6283 40.9539 0.7212

J1246+22 0.47383 0.100E+01 191.6583 22.8833 3850 12.3600 x23.2128 0.7752

J1249x6507 0.43444 0.121Ex16 192.4762 x65.1222 3831 12.2933 66.0512 0.9468

B1254x10 0.61731 0.363Ex15 194.2696 x10.4516 4485 14.3700 9.5197 0.9373

B1257+12 0.00622 0.114Ex18 195.0125 12.6824 4699 15.0942 x13.5992 0.9204

J1301x6305 0.18453 0.267Ex12 195.4404 x63.0928 4650 14.9354 62.2591 0.9747

J1301x6305 0.18453 0.267Ex12 195.4404 x63.0928 4740 15.2225 62.9238 0.2758

J1301x6305 0.18453 0.267Ex12 195.4404 x63.0928 4872 15.6579 62.3448 0.7789

J1301x6310 0.66383 0.564Ex13 195.3679 x63.1779 4740 15.2225 62.9238 0.2928

J1301x6310 0.66383 0.564Ex13 195.3679 x63.1779 4872 15.6579 62.3448 0.8821

J1302x63 0.32572 0.100E+01 195.5167 x63.7481 4740 15.2225 62.9238 0.8752

J1302x63 0.32572 0.100E+01 195.5167 x63.7481 5106 16.3587 63.7217 0.8425

J1302x6313 0.96785 0.633Ex14 195.5800 x63.2247 4740 15.2225 62.9238 0.4673

J1302x6313 0.96785 0.633Ex14 195.5800 x63.2247 4872 15.6579 62.3448 0.8833

J1302x6313 0.96785 0.633Ex14 195.5800 x63.2247 5106 16.3587 63.7217 0.9238

B1259x63 0.04776 0.228Ex14 195.6983 x63.8357 5106 16.3587 63.7217 0.6702

J1303x6305 2.30664 0.218Ex14 195.7500 x63.0836 4740 15.2225 62.9238 0.5512

J1303x6305 2.30664 0.218Ex14 195.7500 x63.0836 4872 15.6579 62.3448 0.7444

J1303x6305 2.30664 0.218Ex14 195.7500 x63.0836 5106 16.3587 63.7217 0.8819

J1305x6203 0.42776 0.321Ex13 196.3371 x62.0560 4872 15.6579 62.3448 0.7380

J1305x6256 0.47823 0.211Ex14 196.3667 x62.9442 4872 15.6579 62.3448 0.9282

J1305x6256 0.47823 0.211Ex14 196.3667 x62.9442 5106 16.3587 63.7217 0.7776

B1302x64 0.57165 0.403Ex14 196.3487 x64.9240 4904 15.7346 64.8363 0.6204

J1307x6318 4.96243 0.211Ex13 196.9779 x63.3097 5106 16.3587 63.7217 0.7437

B1309x12 0.44752 0.151Ex15 197.9692 x12.4671 5407 17.2962 12.6930 0.7098

B1310+18 0.03316 0.100E+01 198.2292 18.1667 5892 18.9267 x18.4161 0.7408

B1310+18 0.03316 0.100E+01 198.2292 18.1667 5968 19.1804 x18.1537 0.9513

J1313+0931 0.84893 0.800Ex15 198.3458 9.5322 5644 18.1242 x9.2237 0.3799

J1320x3512 0.45849 0.190Ex17 200.0525 x35.2072 6176 19.8087 35.7790 0.6216

B1317x53 0.27973 0.925Ex14 200.2246 x53.9851 6465 20.7921 53.4729 0.7645

J1322x6329 2.76421 0.111Ex13 200.5750 x63.4936 6619 21.2442 63.8819 0.7737

J1324x6302 2.48380 0.979Ex15 201.0567 x63.0392 6619 21.2442 63.8819 0.8634

B1323x63 0.79267 0.310Ex14 201.6358 x64.1456 6596 21.1775 64.6000 0.6454

B1323x63 0.79267 0.310Ex14 201.6358 x64.1456 6619 21.2442 63.8819 0.4721

J1327x6400 0.28068 0.312Ex13 201.7925 x64.0036 6596 21.1775 64.6000 0.8567

J1327x6400 0.28068 0.312Ex13 201.7925 x64.0036 6619 21.2442 63.8819 0.5617

B1325x43 0.53270 0.301Ex14 202.0267 x43.9623 6711 21.5775 43.4579 0.6754

J1332x3032 0.65043 0.560Ex15 203.2184 x30.5381 6948 22.3650 30.8948 0.9249

J1332x3032 0.65043 0.560Ex15 203.2184 x30.5381 6978 22.4633 31.0073 0.8889

J1335x3642 0.39919 0.100E+01 203.9000 x36.7000 7728 24.8758 36.6966 0.9758

J1347x5947 0.60996 0.142Ex13 206.8304 x59.7944 8288 26.6967 59.1562 0.6520

J1355x5925 1.21338 0.599Ex14 208.9962 x59.4169 8865 28.5083 59.5492 0.5055

J1358x2533 0.91297 0.100E+01 209.6750 x25.5500 9255 29.7429 26.1484 0.6022

B1356x60 0.12750 0.634Ex14 209.9925 x60.6356 9360 30.0642 59.9073 0.7318

J1406x5806 0.28835 0.611Ex15 211.5050 x58.1089 9857 31.7029 58.1373 0.1999

J1406x6121 0.21307 0.547Ex13 211.7083 x61.3577 9704 31.2029 60.5063 0.9902

J1407x6048 0.49234 0.316Ex14 211.9942 x60.8163 9704 31.2029 60.5063 0.8498

J1407x6048 0.49234 0.316Ex14 211.9942 x60.8163 9726 31.2787 60.3457 0.8563

J1412x6111 0.52916 0.191Ex14 213.2483 x61.1918 10 575 34.0292 60.6302 0.9618

J1416x6037 0.29558 0.428Ex14 214.1271 x60.6332 10 575 34.0292 60.6302 0.0980

J1416x6037 0.29558 0.428Ex14 214.1271 x60.6332 10 677 34.3458 61.3518 0.7512

J1418x3921 1.09681 0.889Ex15 214.7092 x39.3551 10 735 34.5421 39.3278 0.1693

B1417x54 0.93577 0.237Ex15 215.1212 x54.2731 10 960 35.3025 53.5609 0.7348

J1420x6048 0.06818 0.832Ex13 215.0341 x60.8046 10 677 34.3458 61.3518 0.8794

J1425x6210 0.50173 0.480Ex15 216.2821 x62.1680 11 118 35.7529 62.2166 0.5314

J1425x6210 0.50173 0.480Ex15 216.2821 x62.1680 11 156 35.8783 61.7737 0.5644

J1434x6006 0.30637 0.302Ex14 218.5221 x60.1081 11 706 37.7621 60.7114 0.9704

J1434x6029 0.96335 0.103Ex14 218.6629 x60.4969 11 706 37.7621 60.7114 0.9260

J1452x6036 0.15499 0.145Ex14 223.2158 x60.6087 13 447 43.2933 61.0969 0.4943

W.H. Edmondson and I.R. Stevens244

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J1452x6036 0.15499 0.145Ex14 223.2158 x60.6087 13 460 43.3262 60.8535 0.2685

J1454x5846 0.04525 0.817Ex18 223.5454 x58.7763 13 771 44.3063 58.3612 0.8667

B1454x51 1.74830 0.529Ex14 224.4171 x51.3814 13 664 43.9833 51.7060 0.5418

J1457x5900 1.49864 0.366Ex14 224.4125 x59.0142 13 771 44.3063 58.3612 0.6615

J1457x5902 0.39074 0.123Ex13 224.3829 x59.0344 13 771 44.3063 58.3612 0.6775

B1503x51 0.84074 0.637Ex14 226.6646 x51.9694 14 182 45.7192 52.2499 0.9861

B1504x43 0.28676 0.160Ex14 226.8921 x43.8676 14 582 47.0658 44.2060 0.3804

B1508+55 0.73968 0.500Ex14 227.3567 55.5257 14 788 47.7471 x55.1617 0.5338

J1509x6015 0.33904 0.212Ex14 227.2812 x60.2552 14 687 47.4317 60.2386 0.1513

B1507x44 0.94387 0.610Ex15 227.7038 x44.3686 14 582 47.0658 44.2060 0.6583

B1507x44 0.94387 0.610Ex15 227.7038 x44.3686 14 922 48.1258 43.8606 0.6604

B1508x57 0.12869 0.685Ex14 228.1792 x57.9999 15 220 49.0554 58.1682 0.8922

J1513x5739 0.97346 0.276Ex13 228.4954 x57.6504 15 220 49.0554 58.1682 0.7627

J1514x5925 0.14880 0.288Ex14 228.7462 x59.4287 15 202 48.9946 60.2007 0.8110

J1515x5720 0.28665 0.610Ex14 228.7888 x57.3469 15 220 49.0554 58.1682 0.8634

J1517x4356 0.65084 0.216Ex15 229.3638 x43.9383 15 591 50.2029 43.9791 0.8402

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 15 256 49.1958 x2.5839 0.6600

B1516+02B 0.00795 x0.333Ex20 229.6308 2.0876 15 500 49.9346 x2.0715 0.3042

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 15 256 49.1958 x2.5839 0.6627

B1516+02A 0.00555 0.412Ex19 229.6387 2.0910 15 500 49.9346 x2.0715 0.2965

J1531x4012 0.35685 0.963Ex16 232.7833 x40.2086 16 343 52.6583 40.3194 0.1671

J1532x5308 0.44383 0.650Ex16 233.1479 x53.1350 16 612 53.4479 52.2883 0.8983

J1535x5450 0.56673 0.143Ex13 233.9925 x54.8406 16 514 53.1588 55.1853 0.9022

J1535x5848 0.30718 0.272Ex14 233.8196 x58.8077 16 581 53.3608 59.4175 0.7631

J1536x44 0.46842 0.100E+01 234.0625 x44.2667 16 906 54.3867 45.0542 0.8516

B1534+12 0.03790 0.242Ex17 234.2913 11.9321 16 681 53.6587 x12.2977 0.7306

J1537x49 0.30131 0.100E+01 234.3750 x49.1500 17 104 54.9646 49.9358 0.9824

J1537x5153 1.52812 0.417Ex14 234.3154 x51.8850 16 612 53.4479 52.2883 0.9567

J1537x5153 1.52812 0.417Ex14 234.3154 x51.8850 16 973 54.5804 52.5991 0.7617

J1542x5034 0.59925 0.397Ex14 235.6892 x50.5671 17 104 54.9646 49.9358 0.9610

J1542x5034 0.59925 0.397Ex14 235.6892 x50.5671 17 231 55.3567 50.8214 0.4186

J1542x5034 0.59925 0.397Ex14 235.6892 x50.5671 17 341 55.6729 51.1736 0.6068

J1542x5303 1.20757 0.778Ex13 235.7271 x53.0614 17 033 54.7767 52.8191 0.9808

B1540x06 0.70906 0.880Ex15 235.8754 x6.3459 17 332 55.6454 6.9869 0.6811

J1543x5013 0.64425 0.101Ex13 235.9925 x50.2328 17 231 55.3567 50.8214 0.8665

J1543x5013 0.64425 0.101Ex13 235.9925 x50.2328 17 341 55.6729 51.1736 0.9936

J1547x5839 0.24219 0.594Ex15 236.8954 x58.6527 17 568 56.4354 58.8561 0.5029

J1547x5839 0.24219 0.594Ex15 236.8954 x58.6527 17 790 57.1246 57.7676 0.9143

J1547x5839 0.24219 0.594Ex15 236.8954 x58.6527 17 887 57.3950 58.7683 0.5128

J1548x4927 0.60274 0.405Ex14 237.0808 x49.4612 18 004 57.7392 49.4743 0.6585

J1548x5607 0.17093 0.107Ex13 237.1833 x56.1261 18 002 57.7312 55.3486 0.9511

J1548x5607 0.17093 0.107Ex13 237.1833 x56.1261 18 023 57.7663 56.1077 0.5832

J1549+21 1.26247 0.100E+01 237.4208 21.2500 18 191 58.3762 x21.0135 0.9842

J1549x4848 0.28835 0.141Ex13 237.3379 x48.8104 18 004 57.7392 49.4743 0.7758

J1549x5722 0.49777 0.470Ex16 237.4496 x57.3672 17 790 57.1246 57.7676 0.5157

J1550x5242 0.74966 0.178Ex13 237.5121 x52.7019 17 800 57.1562 51.8234 0.9479

J1550x5242 0.74966 0.178Ex13 237.5121 x52.7019 18 207 58.4058 52.5630 0.9045

B1550x54 1.08133 0.156Ex13 238.4983 x54.9350 18 002 57.7312 55.3486 0.8715

B1550x54 1.08133 0.156Ex13 238.4983 x54.9350 18 256 58.5767 54.9044 0.0841

J1554x5512 3.41804 0.312Ex13 238.6687 x55.2092 18 002 57.7312 55.3486 0.9478

J1554x5512 3.41804 0.312Ex13 238.6687 x55.2092 18 256 58.5767 54.9044 0.3184

B1552x31 0.51811 0.622Ex16 238.8246 x31.5723 18 204 58.3979 30.7735 0.9056

J1556x5358 0.99468 0.104Ex13 239.2146 x53.9819 18 351 58.8458 53.5575 0.5622

B1556x57 0.19445 0.213Ex14 240.0829 x57.8541 18 567 59.6225 58.6195 0.8932

J1601x5244 2.55936 0.720Ex15 240.3638 x52.7358 18 712 60.1192 52.9474 0.3234

J1601x5244 2.55936 0.720Ex15 240.3638 x52.7358 18 966 60.9629 53.2777 0.8079

J1601x5335 0.28846 0.624Ex13 240.4787 x53.5953 18 712 60.1192 52.9474 0.7410

J1601x5335 0.28846 0.624Ex13 240.4787 x53.5953 18 966 60.9629 53.2777 0.5791

B1601x52 0.65801 0.256Ex15 241.3179 x52.9509 18 966 60.9629 53.2777 0.4825

B1604x00 0.42182 0.306Ex15 241.8004 x0.5447 19 386 62.2875 0.1789 0.6091

J1610x5006 0.48112 0.136Ex13 242.6846 x50.1117 19 581 62.9437 49.7460 0.4482

J1611x4949 0.66644 0.540Ex15 242.9442 x49.8326 19 581 62.9437 49.7460 0.0865

B1609x47 0.38238 0.632Ex15 243.3708 x47.2405 19 553 62.8200 46.9206 0.6370

Utilization of pulsars 245

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J1613x5234 0.65522 0.663Ex14 243.4892 x52.5671 20 028 64.4367 52.3727 0.9672

B1612+07 1.20680 0.236Ex14 243.6704 7.6253 19 987 64.3058 x7.3942 0.6761

J1614x5144 1.53401 0.744Ex14 243.6904 x51.7347 20 028 64.4367 52.3727 0.9818

J1616x5208 1.02583 0.289Ex13 244.0975 x52.1347 20 028 64.4367 52.3727 0.4144

J1621x5243 0.37192 0.768Ex15 245.4825 x52.7179 20 434 65.6558 51.9418 0.7952

J1622x4802 0.26507 0.307Ex15 245.6962 x48.0370 20 359 65.3996 48.3370 0.4219

B1620x09 1.27645 0.258Ex14 245.8233 x9.1470 20 273 65.1829 8.4093 0.9769

B1620x09 1.27645 0.258Ex14 245.8233 x9.1470 20 447 65.7121 9.7715 0.6343

B1620x26 0.01108 0.671Ex18 245.9091 x26.5316 20 626 66.2946 25.7493 0.8721

B1620x26 0.01108 0.671Ex18 245.9091 x26.5316 20 652 66.3783 26.2924 0.5266

B1620x42 0.36459 0.102Ex14 245.9512 x42.9348 20 753 66.7054 42.9099 0.7546

J1624x4721 0.44872 0.415Ex14 246.2283 x47.3507 20 800 66.8525 46.8539 0.7978

J1625x4048 2.35528 0.443Ex15 246.2929 x40.8060 20 550 66.0462 40.9609 0.2913

J1626x4537 0.37014 0.828Ex14 246.7038 x45.6238 20 494 65.8862 45.0791 0.9824

J1626x4537 0.37014 0.828Ex14 246.7038 x45.6238 20 861 67.0558 45.0457 0.6769

J1627+1419 0.49086 0.393Ex15 246.8279 14.3224 20 915 67.2450 x13.6612 0.7818

J1627x5547 0.35246 0.738Ex15 246.8375 x55.7979 20 910 67.2262 55.0005 0.8871

J1630x4719 0.55907 0.142Ex13 247.5100 x47.3178 20 800 66.8525 46.8539 0.8047

B1633+24 0.49051 0.119Ex15 248.8571 24.3133 21 354 68.7275 x25.0389 0.7371

J1635x4513 1.59475 0.360Ex14 248.9808 x45.2174 21 701 69.8908 45.6204 0.9952

J1635x4944 0.67196 0.879Ex14 248.9808 x49.7343 21 552 69.4125 49.8604 0.4497

B1630x59 0.52912 0.137Ex14 248.7875 x59.9011 21 384 68.8408 60.7449 0.8454

J1636x4803 1.20464 0.207Ex13 249.1333 x48.0515 21 496 69.2546 47.7583 0.3173

J1636x4933 0.43037 0.151Ex14 249.2296 x49.5503 21 552 69.4125 49.8604 0.3600

B1634x45 0.11877 0.319Ex14 249.4946 x45.8909 21 701 69.8908 45.6204 0.4798

J1637x4721 1.16574 0.444Ex14 249.2975 x47.3501 21 496 69.2546 47.7583 0.4104

J1638x4608 0.27814 0.515Ex13 249.5954 x46.1366 21 701 69.8908 45.6204 0.5947

J1638x5226 0.34050 0.265Ex14 249.7496 x52.4493 21 553 69.4192 52.8948 0.5547

B1635x45 0.26456 0.289Ex14 249.8383 x46.0759 21 701 69.8908 45.6204 0.4585

J1640x4648 0.17835 0.806Ex15 250.1983 x46.8013 22 032 71.0458 46.9657 0.8633

B1636x47 0.51740 0.420Ex13 250.0546 x47.2598 21 496 69.2546 47.7583 0.9426

J1640x4951 0.73910 0.334Ex15 250.1812 x49.8506 21 552 69.4125 49.8604 0.7688

J1640x4951 0.73910 0.334Ex15 250.1812 x49.8506 21 807 70.2704 50.0665 0.2336

B1639+36A 0.01038 0.100E+01 250.4200 36.4543 21 724 69.9637 x35.6440 0.9299

B1639+36A 0.01038 0.100E+01 250.4200 36.4543 21 872 70.5371 x35.4761 0.9851

B1639+36B 0.00353 0.100E+01 250.4208 36.4500 21 724 69.9637 x35.6440 0.9266

B1639+36B 0.00353 0.100E+01 250.4208 36.4500 21 872 70.5371 x35.4761 0.9808

J1641x2347 1.09101 0.411Ex16 250.3250 x23.7843 21 788 70.2042 23.8097 0.1235

J1641x2347 1.09101 0.411Ex16 250.3250 x23.7843 21 868 70.5242 23.0602 0.7510

J1641x2347 1.09101 0.411Ex16 250.3250 x23.7843 21 961 70.8071 24.0890 0.5703

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 21 918 70.7029 12.2103 0.2912

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 22 012 70.9729 12.6858 0.2770

J1643x1224 0.00462 0.185Ex19 250.9088 x12.4163 22 021 71.0154 12.9912 0.5847

J1643x4522 1.34790 0.828Ex14 250.8350 x45.3667 21 701 69.8908 45.6204 0.9777

J1643x4550 0.71751 0.300Ex13 250.8063 x45.8485 21 701 69.8908 45.6204 0.9434

B1641x45 0.45506 0.201Ex13 251.2050 x45.9860 22 032 71.0458 46.9657 0.9925

J1645+1012 0.41086 0.813Ex16 251.3933 10.2044 22 288 72.0042 x10.9334 0.9510

B1642x03 0.38769 0.178Ex14 251.2583 x3.2996 22 177 71.5779 3.6363 0.4643

J1648x3256 0.71946 0.353Ex14 252.0250 x32.9447 22 217 71.6650 32.6318 0.4769

J1648x3256 0.71946 0.353Ex14 252.0250 x32.9447 22 559 72.8196 32.8902 0.7964

J1649+2533 1.01526 0.600Ex15 252.4342 25.5502 22 668 73.1450 x25.9945 0.8383

J1649x4729 0.29769 0.655Ex14 252.3259 x47.4848 22 124 71.4200 47.6988 0.9308

J1649x5553 0.61357 0.170Ex14 252.3796 x55.8844 22 569 72.8625 55.8372 0.4852

J1649x5553 0.61357 0.170Ex14 252.3796 x55.8844 22 624 73.0171 56.4234 0.8348

J1650x1654 1.74955 0.320Ex14 252.6133 x16.9115 22 347 72.1717 16.6345 0.5214

J1650x1654 1.74955 0.320Ex14 252.6133 x16.9115 22 782 73.5125 17.0268 0.9065

J1650x4502 0.38087 0.161Ex13 252.6346 x45.0437 22 638 73.0558 44.9740 0.4270

B1648x17 0.97339 0.304Ex14 252.8821 x17.1506 22 347 72.1717 16.6345 0.8781

B1648x17 0.97339 0.304Ex14 252.8821 x17.1506 22 782 73.5125 17.0268 0.6424

B1648x17 0.97339 0.304Ex14 252.8821 x17.1506 22 805 73.5858 17.6092 0.8400

J1651x4519 0.51744 0.819Ex14 252.9883 x45.3170 22 638 73.0558 44.9740 0.3496

J1651x4519 0.51744 0.819Ex14 252.9883 x45.3170 22 817 73.6388 45.6811 0.7454

B1647x52 0.63506 0.181Ex14 252.9288 x52.3828 22 695 73.1942 51.5429 0.8809

W.H. Edmondson and I.R. Stevens246

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B1647x528 0.89053 0.207Ex14 252.9217 x52.9180 22 429 72.3883 53.3659 0.6964

J1652+2651 0.91580 0.650Ex15 253.0125 26.8611 22 668 73.1450 x25.9945 0.8767

B1649x23 1.70374 0.316Ex14 253.2438 x24.0514 22 557 72.8117 24.2908 0.4940

B1649x23 1.70374 0.316Ex14 253.2438 x24.0514 22 729 73.3417 24.1774 0.1596

B1649x23 1.70374 0.316Ex14 253.2438 x24.0514 22 801 73.5704 23.9829 0.3338

B1650x38 0.30504 0.279Ex14 253.4154 x38.6391 22 760 73.4542 38.7720 0.1384

J1653x4249 0.61256 0.481Ex14 253.4175 x42.8176 22 915 73.9683 43.1557 0.6463

J1653x4315 0.41928 0.150Ex16 253.3737 x43.2500 22 915 73.9683 43.1557 0.6020

J1654x2713 0.79182 0.168Ex15 253.5979 x27.2183 22 600 72.9379 26.8623 0.7499

J1654x2713 0.79182 0.168Ex15 253.5979 x27.2183 22 802 73.5746 26.8077 0.4112

J1654x2713 0.79182 0.168Ex15 253.5979 x27.2183 22 920 73.9825 27.8356 0.7273

J1654x2713 0.79182 0.168Ex15 253.5979 x27.2183 23 056 74.4196 27.3761 0.8367

J1658x4306 1.16645 0.428Ex13 254.5692 x43.1014 22 915 73.9683 43.1557 0.6033

B1657x13 0.64096 0.618Ex15 254.9708 x13.0858 23 085 74.5271 13.0350 0.4467

J1700x3312 1.35831 0.471Ex14 255.2208 x33.2125 23 269 75.1004 33.7343 0.5355

J1700x4939 0.57836 0.108Ex14 255.0938 x49.6504 23 198 74.8829 48.7799 0.8957

J1700x4939 0.57836 0.108Ex14 255.0938 x49.6504 23 307 75.1875 48.8146 0.8410

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 291 75.1533 29.4729 0.6526

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 302 75.1750 30.8972 0.7990

J1701x3006A 0.00524 x0.132Ex18 255.3021 x30.1084 23 438 75.5733 29.9950 0.2940

J1701x3006B 0.00359 x0.350Ex18 255.3025 x30.1136 23 291 75.1533 29.4729 0.6579

J1701x3006B 0.00359 x0.350Ex18 255.3025 x30.1136 23 302 75.1750 30.8972 0.7939

J1701x3006B 0.00359 x0.350Ex18 255.3025 x30.1136 23 438 75.5733 29.9950 0.2957

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 291 75.1533 29.4729 0.6609

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 302 75.1750 30.8972 0.7911

J1701x3006C 0.00381 x0.320Ex19 255.3033 x30.1165 23 438 75.5733 29.9950 0.2961

J1701x3006D 0.00342 0.100E+01 255.3000 x30.1000 23 291 75.1533 29.4729 0.6440

J1701x3006D 0.00342 0.100E+01 255.3000 x30.1000 23 302 75.1750 30.8972 0.8069

J1701x3006D 0.00342 0.100E+01 255.3000 x30.1000 23 438 75.5733 29.9950 0.2928

J1701x3006E 0.00323 0.100E+01 255.3000 x30.1000 23 291 75.1533 29.4729 0.6440

J1701x3006E 0.00323 0.100E+01 255.3000 x30.1000 23 302 75.1750 30.8972 0.8069

J1701x3006E 0.00323 0.100E+01 255.3000 x30.1000 23 438 75.5733 29.9950 0.2928

J1701x3006F 0.00230 0.100E+01 255.3000 x30.1000 23 291 75.1533 29.4729 0.6440

J1701x3006F 0.00230 0.100E+01 255.3000 x30.1000 23 302 75.1750 30.8972 0.8069

J1701x3006F 0.00230 0.100E+01 255.3000 x30.1000 23 438 75.5733 29.9950 0.2928

J1701x3130 0.29134 0.560Ex16 255.4312 x31.5102 23 205 74.9025 31.5852 0.5340

J1701x3130 0.29134 0.560Ex16 255.4312 x31.5102 23 302 75.1750 30.8972 0.6644

J1701x3130 0.29134 0.560Ex16 255.4312 x31.5102 23 409 75.4638 31.6327 0.1267

J1702x4310 0.24052 0.224Ex12 255.6121 x43.1678 23 655 76.2592 43.3133 0.6632

B1700x18 0.80434 0.173Ex14 255.9625 x18.7710 23 579 76.0400 19.0947 0.3328

J1703x4851 1.39640 0.508Ex14 255.9767 x48.8655 23 307 75.1875 48.8146 0.7908

B1702x19 0.29899 0.414Ex14 256.4004 x19.1107 23 579 76.0400 19.0947 0.3608

J1705x3423 0.25543 0.108Ex14 256.4262 x34.3957 23 797 76.6967 34.5355 0.3044

J1705x3950 0.31894 0.606Ex13 256.3742 x39.8350 23 764 76.6237 40.6142 0.8182

J1705x4108 0.86107 0.347Ex13 256.3350 x41.1346 23 764 76.6237 40.6142 0.5951

J1706x4310 0.61698 0.651Ex14 256.5187 x43.1673 23 655 76.2592 43.3133 0.2978

B1703x40 0.58102 0.192Ex14 256.8404 x40.8989 23 764 76.6237 40.6142 0.3578

B1703x40 0.58102 0.192Ex14 256.8404 x40.8989 24 096 77.6417 40.8441 0.8031

J1707x4341 0.89059 0.570Ex14 256.9171 x43.6867 23 655 76.2592 43.3133 0.7565

J1708x3426 0.69211 0.420Ex14 257.2404 x34.4465 23 797 76.6967 34.5355 0.5510

J1708x4008 10.99903 0.194Ex10 257.1958 x40.1508 23 764 76.6237 40.6142 0.7362

J1708x4008 10.99903 0.194Ex10 257.1958 x40.1508 24 096 77.6417 40.8441 0.8243

B1706x16 0.65305 0.631Ex14 257.3600 x16.6826 23 847 76.9025 15.9682 0.8484

B1706x16 0.65305 0.631Ex14 257.3600 x16.6826 24 142 77.7742 17.3994 0.8279

B1706x16 0.65305 0.631Ex14 257.3600 x16.6826 24 292 78.1996 16.3077 0.9195

J1710x4148 0.28656 0.102Ex15 257.5988 x41.8005 24 096 77.6417 40.8441 0.9573

J1710x4148 0.28656 0.102Ex15 257.5988 x41.8005 24 243 78.0721 41.4471 0.5907

B1709x15 0.86880 0.110Ex14 257.9792 x15.1611 24 104 77.6662 15.2796 0.3346

J1712x2715 0.25536 0.128Ex14 258.0488 x27.2515 24 304 78.2308 27.7738 0.5532

J1712x2715 0.25536 0.128Ex14 258.0488 x27.2515 24 370 78.4379 27.2401 0.3893

J1712x2715 0.25536 0.128Ex14 258.0488 x27.2515 24 546 78.9875 27.1280 0.9468

J1713+0747 0.00457 0.854Ex20 258.4563 7.7937 24 353 78.3862 x7.3299 0.4691

J1713+0747 0.00457 0.854Ex20 258.4563 7.7937 24 472 78.7825 x7.3458 0.5542

Utilization of pulsars 247

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J1713x3949 0.39200 0.100E+01 258.3667 x39.8167 24 583 79.1133 39.8586 0.7478

J1715x3700 0.77963 0.150Ex15 258.7900 x37.0001 24 332 78.3229 37.3376 0.5763

J1715x3903 0.27848 0.377Ex13 258.8096 x39.0501 24 583 79.1133 39.8586 0.8637

J1715x4034 2.07215 0.301Ex14 258.9204 x40.5673 24 583 79.1133 39.8586 0.7345

J1716x3720 0.63031 0.180Ex13 259.0471 x37.3346 24 332 78.3229 37.3376 0.7242

J1717x4043 0.39786 0.122Ex13 259.4496 x40.7181 24 583 79.1133 39.8586 0.9229

J1717x40433 0.34993 0.175Ex14 259.2583 x40.7175 24 583 79.1133 39.8586 0.8711

J1717x5800 0.32179 0.196Ex15 259.3983 x58.0015 24 801 79.7550 58.1099 0.3727

B1715x40 0.18909 0.167Ex14 259.7571 x40.1165 24 583 79.1133 39.8586 0.6935

J1720+2150 1.61566 0.700Ex15 260.0054 21.8337 24 862 79.9458 x22.5431 0.7118

B1718x02 0.47771 0.828Ex16 260.2383 x2.2066 24 864 79.9542 2.5139 0.4185

B1717x29 0.62045 0.746Ex15 260.1421 x29.5545 25 141 80.7054 28.7469 0.9846

B1718x35 0.28042 0.252Ex13 260.3863 x35.5471 25 030 80.3979 34.7441 0.8032

B1718x32 0.47716 0.646Ex15 260.5121 x32.1292 24 877 80.0029 32.7857 0.8308

J1724x3505 1.22171 0.211Ex13 261.1992 x35.0843 25 030 80.3979 34.7441 0.8705

B1726x00 0.38600 0.112Ex14 262.1450 x0.1292 25 905 82.9342 0.0999 0.7897

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 25 586 82.0250 22.9307 0.5832

J1730x2304 0.00812 0.202Ex19 262.5900 x23.0754 25 652 82.1992 23.9581 0.9653

J1732x1930 0.48377 0.182Ex15 263.0829 x19.5005 26 018 83.2788 20.0363 0.5705

J1732x5049 0.00531 0.138Ex19 263.1988 x50.8167 26 113 83.5362 51.2162 0.5230

B1730x22 0.87168 0.427Ex16 263.3600 x22.4677 26 159 83.6521 21.6223 0.8945

B1730x22 0.87168 0.427Ex16 263.3600 x22.4677 26 328 84.1100 21.9933 0.8875

J1735x3258 0.35096 0.261Ex13 263.9871 x32.9672 26 326 84.1042 32.0037 0.9706

J1736x3511 0.50280 0.157Ex14 264.0113 x35.1849 26 290 83.9800 35.5076 0.3242

J1736x3511 0.50280 0.157Ex14 264.0113 x35.1849 26 506 84.5533 35.9772 0.9600

J1737x3102 0.76867 0.373Ex13 264.3904 x31.0335 26 419 84.3404 31.3314 0.3021

J1737x3102 0.76867 0.373Ex13 264.3904 x31.0335 26 550 84.6867 30.2240 0.8620

J1737x3102 0.76867 0.373Ex13 264.3904 x31.0335 26 650 84.9604 31.2241 0.6010

J1737x3137 0.45043 0.139Ex12 264.2675 x31.6173 26 326 84.1042 32.0037 0.4195

J1737x3137 0.45043 0.139Ex12 264.2675 x31.6173 26 419 84.3404 31.3314 0.2950

J1737x3137 0.45043 0.139Ex12 264.2675 x31.6173 26 650 84.9604 31.2241 0.7967

B1734x35 0.39759 0.612Ex14 264.4167 x35.9288 26 290 83.9800 35.5076 0.6067

B1734x35 0.39759 0.612Ex14 264.4167 x35.9288 26 506 84.5533 35.9772 0.1450

J1738x2955 0.44340 0.819Ex13 264.7175 x29.9181 26 550 84.6867 30.2240 0.3075

B1735x32 0.76850 0.795Ex15 264.7254 x32.1982 26 326 84.1042 32.0037 0.6510

B1735x32 0.76850 0.795Ex15 264.7254 x32.1982 26 419 84.3404 31.3314 0.9485

B1735x32 0.76850 0.795Ex15 264.7254 x32.1982 26 744 85.2408 32.8960 0.8675

B1735x32 0.76850 0.795Ex15 264.7254 x32.1982 26 863 85.5521 31.8734 0.8882

J1739x3023 0.11437 0.114Ex13 264.9158 x30.3837 26 550 84.6867 30.2240 0.2793

J1739x3023 0.11437 0.114Ex13 264.9158 x30.3837 26 650 84.9604 31.2241 0.8416

J1739x3049 0.23932 0.218Ex14 264.8467 x30.8178 26 419 84.3404 31.3314 0.7212

J1739x3049 0.23932 0.218Ex14 264.8467 x30.8178 26 550 84.6867 30.2240 0.6150

J1739x3049 0.23932 0.218Ex14 264.8467 x30.8178 26 650 84.9604 31.2241 0.4219

B1736x31 0.52944 0.186Ex13 264.8513 x31.5209 26 326 84.1042 32.0037 0.8895

B1736x31 0.52944 0.186Ex13 264.8513 x31.5209 26 419 84.3404 31.3314 0.5449

B1736x31 0.52944 0.186Ex13 264.8513 x31.5209 26 650 84.9604 31.2241 0.3163

B1736x31 0.52944 0.186Ex13 264.8513 x31.5209 26 863 85.5521 31.8734 0.7845

J1739x3159 0.87756 0.197Ex15 264.9525 x31.9847 26 326 84.1042 32.0037 0.8485

J1739x3159 0.87756 0.197Ex15 264.9525 x31.9847 26 419 84.3404 31.3314 0.8952

J1739x3159 0.87756 0.197Ex15 264.9525 x31.9847 26 650 84.9604 31.2241 0.7607

J1739x3159 0.87756 0.197Ex15 264.9525 x31.9847 26 744 85.2408 32.8960 0.9558

J1739x3159 0.87756 0.197Ex15 264.9525 x31.9847 26 863 85.5521 31.8734 0.6098

J1740+1000 0.15409 0.215Ex13 265.1079 10.0017 26 670 85.0208 x10.7322 0.7356

J1740+1000 0.15409 0.215Ex13 265.1079 10.0017 27 058 86.0729 x10.0164 0.9651

B1737+13 0.80305 0.145Ex14 265.0304 13.1991 26 654 84.9733 x13.8699 0.6732

B1737x30 0.60667 0.466Ex12 265.1408 x30.2621 26 550 84.6867 30.2240 0.4557

B1737x30 0.60667 0.466Ex12 265.1408 x30.2621 26 650 84.9604 31.2241 0.9788

J1740x3052 0.57031 0.255Ex13 265.2083 x30.8678 26 419 84.3404 31.3314 0.9840

J1740x3052 0.57031 0.255Ex13 265.2083 x30.8678 26 550 84.6867 30.2240 0.8286

J1740x3052 0.57031 0.255Ex13 265.2083 x30.8678 26 650 84.9604 31.2241 0.4341

J1740x5340 0.00365 0.168Ex18 265.1854 x53.6780 26 871 85.5804 53.5156 0.4271

J1740x5340 0.00365 0.168Ex18 265.1854 x53.6780 26 933 85.7446 54.2576 0.8054

J1741+2758 1.36074 0.184Ex14 265.4725 27.9669 26 731 85.1942 x28.2734 0.4140

W.H. Edmondson and I.R. Stevens248

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B1738x08 2.04308 0.227Ex14 265.3438 x8.6755 26 729 85.1929 9.2656 0.6091

J1741x2019 3.90451 0.163Ex13 265.2783 x20.3173 26 568 84.7321 20.0306 0.6169

J1741x2019 3.90451 0.163Ex13 265.2783 x20.3173 26 951 85.7825 20.0730 0.5603

J1741x2945 0.22356 0.634Ex15 265.3100 x29.7510 26 550 84.6867 30.2240 0.7825

J1741x3016 1.89375 0.899Ex14 265.2791 x30.2675 26 550 84.6867 30.2240 0.5941

B1737x39 0.51221 0.193Ex14 265.3250 x39.4607 26 909 85.6942 40.2434 0.8654

B1740x03 0.44464 0.156Ex14 265.7838 x3.6532 26 615 84.8621 3.4165 0.9516

B1740x31 2.41458 0.121Ex12 265.9025 x31.8394 26 863 85.5521 31.8734 0.3521

J1743x3153 0.19310 0.106Ex13 265.8146 x31.8848 26 863 85.5521 31.8734 0.2627

J1743x4212 0.30617 0.783Ex15 265.7717 x42.2007 27 251 86.6329 42.0739 0.8705

J1744x3130 1.06606 0.212Ex13 266.0233 x31.5001 26 863 85.5521 31.8734 0.6012

J1746+2540 1.05815 0.800Ex15 266.5275 25.6677 26 977 85.8687 x25.6220 0.6603

J1746+2540 1.05815 0.800Ex15 266.5275 25.6677 27 292 86.7467 x25.7067 0.2226

J1747x2958 0.09881 0.614Ex13 266.8171 x29.9669 27 336 86.8533 29.6579 0.3111

B1745x20 0.28860 0.400Ex15 267.2191 x20.3512 27 495 87.3354 21.0392 0.6978

J1748x2444 0.44284 0.111Ex15 267.2021 x24.7344 27 236 86.5846 25.4764 0.9654

J1748x2444 0.44284 0.111Ex15 267.2021 x24.7344 27 640 87.7604 25.2288 0.7458

B1744x24A 0.01156 x0.340Ex19 267.0092 x24.7769 27 236 86.5846 25.4764 0.8183

B1744x24A 0.01156 x0.340Ex19 267.0092 x24.7769 27 640 87.7604 25.2288 0.8767

J1748x2446C 0.00844 x0.606Ex18 267.0187 24.7677 27 292 86.7467 x25.7067 0.9777

J1749x2629 1.33539 0.172Ex14 267.2967 x26.4836 27 527 87.4400 27.1220 0.6543

B1746x30 0.60987 0.787Ex14 267.3058 x30.0343 27 336 86.8533 29.6579 0.5886

J1750x2438 0.71279 0.108Ex13 267.7487 x24.6349 27 640 87.7604 25.2288 0.5940

J1750x3503 0.68401 0.381Ex16 267.6854 x35.0525 27 361 86.9233 35.5569 0.9139

J1750x3503 0.68401 0.381Ex16 267.6854 x35.0525 27 501 87.3533 35.9819 0.9869

J1751x2516 0.39484 0.264Ex14 267.9691 x25.2679 27 640 87.7604 25.2288 0.2123

J1751x3323 0.54822 0.890Ex14 267.8863 x33.3844 27 528 87.4421 32.9731 0.6053

J1751x3323 0.54822 0.890Ex14 267.8863 x33.3844 27 860 88.4154 33.7377 0.6362

B1747x46 0.74235 0.129Ex14 267.9258 x46.9569 27 372 86.9579 46.9837 0.9683

B1749x28 0.56256 0.813Ex14 268.2442 x28.1104 28 020 88.9000 28.0321 0.6605

J1752x2821 0.64023 0.347Ex14 268.1021 x28.3503 28 020 88.9000 28.0321 0.8590

B1750x24 0.52834 0.141Ex13 268.3775 x25.0007 27 640 87.7604 25.2288 0.6579

B1753+52 2.39140 0.156Ex14 268.5954 52.0201 28 240 89.5108 x52.2047 0.9339

J1755x2725 0.26195 0.140Ex16 268.9242 x27.4179 27 907 88.5783 26.6397 0.8516

J1755x2725 0.26195 0.140Ex16 268.9242 x27.4179 28 020 88.9000 28.0321 0.6147

J1758+3030 0.94726 0.720Ex15 269.6075 30.5067 28 021 88.9021 x29.9170 0.9194

J1758+3030 0.94726 0.720Ex15 269.6075 30.5067 28 396 89.9692 x30.8579 0.5041

J1759x1940 0.25472 0.934Ex16 269.9875 x19.6675 28 312 89.7375 18.9800 0.7315

J1759x1956 2.84339 0.186Ex13 269.8975 x19.9336 28 312 89.7375 18.9800 0.9669

J1759x2549 0.95655 0.996Ex13 269.8963 x25.8169 28 640 90.7188 25.8845 0.8253

J1759x2922 0.57440 0.463Ex14 269.9508 x29.3686 28 411 90.0100 28.7470 0.6244

B1758x03 0.92149 0.331Ex14 270.3441 x3.9653 28 428 90.0575 4.8352 0.9159

J1801x1855 2.55050 0.180Ex15 270.3429 x18.9180 28 312 89.7375 18.9800 0.6086

J1801x1909 1.10872 0.703Ex15 270.4442 x19.1510 28 312 89.7375 18.9800 0.7271

B1757x24 0.12492 0.128Ex12 270.2500 x24.8576 28 791 91.1763 25.1788 0.9803

B1758x29 1.08191 0.329Ex14 270.4450 x29.3441 28 411 90.0100 28.7470 0.7387

J1802x2426 0.56901 0.856Ex14 270.5129 x24.4345 28 791 91.1763 25.1788 0.9970

B1800x21 0.13362 0.134Ex12 270.9637 x21.6008 28 494 90.2246 21.0219 0.9389

B1800x27 0.33441 0.171Ex16 270.8817 x27.2002 28 528 90.3258 27.2816 0.5618

B1802x07 0.02310 0.467Ex18 271.2075 x7.5902 29 063 91.9675 8.2203 0.9872

J1804x2228 0.57051 0.143Ex15 271.1171 x22.4672 29 061 91.9521 22.0028 0.9554

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 28 528 90.3258 27.2816 0.7622

J1804x2717 0.00934 0.409Ex19 271.0879 x27.2920 29 074 91.9958 27.4284 0.9181

B1804x12 0.52262 0.141Ex14 271.5279 x11.9079 29 111 92.0829 11.4595 0.7135

J1806x1920 0.87979 0.170Ex16 271.5275 x19.3340 29 221 92.4246 19.0933 0.9288

J1806x2125 0.48179 0.121Ex12 271.5813 x21.4178 29 061 91.9521 22.0028 0.6926

B1804x08 0.16373 0.288Ex16 271.9083 x8.7953 29 063 91.9675 8.2203 0.5781

B1804x08 0.16373 0.288Ex16 271.9083 x8.7953 29 132 92.1696 9.4782 0.7312

J1807x2459 0.00306 0.100E+01 271.8346 x24.9979 28 791 91.1763 25.1788 0.6827

B1804x27 0.82778 0.122Ex13 271.7850 x27.2508 29 074 91.9958 27.4284 0.2757

J1808x0813 0.87604 0.124Ex14 272.0392 x8.2171 29 063 91.9675 8.2203 0.0717

J1809x0743 0.31389 0.152Ex15 272.3996 x7.7171 29 063 91.9675 8.2203 0.6633

J1809x1917 0.08275 0.255Ex13 272.4296 x19.2939 29 221 92.4246 19.0933 0.2007

Utilization of pulsars 249

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J1809x2004 0.43481 0.728Ex14 272.3158 x20.0670 29 221 92.4246 19.0933 0.9798

B1806x21 0.70241 0.382Ex14 272.3096 x21.1507 29 061 91.9521 22.0028 0.9240

J1809x3547 0.86039 0.120Ex15 272.3621 x35.7838 28 908 91.5358 35.3884 0.9160

J1809x3547 0.86039 0.120Ex15 272.3621 x35.7838 29 504 93.2438 35.3484 0.9833

J1810x1820 0.15372 0.520Ex16 272.7313 x18.3344 29 189 92.3625 17.8345 0.6212

J1810x1820 0.15372 0.520Ex16 272.7313 x18.3344 29 221 92.4246 19.0933 0.8185

J1810x1820 0.15372 0.520Ex16 272.7313 x18.3344 29 248 92.5037 17.9348 0.4599

B1806x53 0.26105 0.383Ex15 272.6850 x53.6355 29 532 93.3254 52.9105 0.9673

J1811x1736 0.10418 0.180Ex17 272.9792 x17.6103 29 189 92.3625 17.8345 0.6562

J1811x1736 0.10418 0.180Ex17 272.9792 x17.6103 29 248 92.5037 17.9348 0.5756

J1811x1835 0.55746 0.631Ex14 272.8737 x18.5846 29 189 92.3625 17.8345 0.9077

J1811x1835 0.55746 0.631Ex14 272.8737 x18.5846 29 221 92.4246 19.0933 0.6786

J1811x1835 0.55746 0.631Ex14 272.8737 x18.5846 29 248 92.5037 17.9348 0.7477

J1811x1925 0.06467 0.440Ex13 272.8717 x19.4174 29 221 92.4246 19.0933 0.5522

B1809x173 1.20537 0.191Ex13 273.0300 x17.3082 29 189 92.3625 17.8345 0.8501

B1809x173 1.20537 0.191Ex13 273.0300 x17.3082 29 248 92.5037 17.9348 0.8183

B1809x176 0.53834 0.982Ex15 273.0659 x17.5511 29 189 92.3625 17.8345 0.7583

B1809x176 0.53834 0.982Ex15 273.0659 x17.5511 29 248 92.5037 17.9348 0.6806

B1811+40 0.93109 0.255Ex14 273.3050 40.2275 29 804 94.1300 x40.5323 0.8795

J1814+1130 0.75126 0.166Ex14 273.6779 11.5122 29 803 94.1188 x11.1432 0.5749

J1814x1649 0.95746 0.633Ex14 273.6554 x16.8174 29 828 94.2200 17.4384 0.8392

J1814x1744 3.97585 0.743Ex12 273.6788 x17.7343 29 828 94.2200 17.4384 0.6168

J1814x1744 3.97585 0.743Ex12 273.6788 x17.7343 29 875 94.3571 17.9894 0.7247

B1813x17 0.78231 0.726Ex14 274.0775 x17.4841 29 828 94.2200 17.4384 0.1496

B1813x17 0.78231 0.726Ex14 274.0775 x17.4841 29 875 94.3571 17.9894 0.5775

B1813x36 0.38702 0.205Ex14 274.2737 x36.3011 29 701 93.8504 36.3579 0.4271

B1813x36 0.38702 0.205Ex14 274.2737 x36.3011 29 910 94.4625 35.3281 0.9912

J1817x3837 0.38449 0.580Ex15 274.2508 x38.6332 29 582 93.5025 38.8417 0.7768

J1818x1519 0.93969 0.411Ex14 274.5608 x15.3179 30 067 94.9171 16.0133 0.7814

J1818x1541 0.55113 0.968Ex14 274.6562 x15.6846 30 067 94.9171 16.0133 0.4196

J1819x1510 0.22654 0.790Ex17 274.9734 x15.1724 30 067 94.9171 16.0133 0.8428

B1817x18 0.30990 0.936Ex16 275.1625 x18.3009 29 875 94.3571 17.9894 0.8636

J1821+17 1.36668 0.870Ex15 275.3058 17.2512 30 232 95.4054 x18.1664 0.9206

J1822+11 1.78700 0.100E+01 275.5708 11.3667 30 114 95.0592 x10.7250 0.8207

B1821+05 0.75291 0.227Ex15 275.8788 5.8401 30 509 96.1975 x5.5036 0.4635

J1823x0154 0.75978 0.113Ex14 275.9671 x1.9013 30 112 95.0550 2.2591 0.9798

J1823x0154 0.75978 0.113Ex14 275.9671 x1.9013 30 585 96.4221 1.1519 0.8767

B1820x11 0.27983 0.138Ex14 275.9179 x11.2503 30 552 96.3346 11.2334 0.4170

J1823x1807 1.63679 0.280Ex15 275.7900 x18.1176 30 220 95.3654 17.2951 0.9256

B1821x11 0.43576 0.355Ex14 276.1229 x11.3118 30 552 96.3346 11.2334 0.2258

J1824x1159 0.36249 0.538Ex14 276.2337 x11.9982 30 552 96.3346 11.2334 0.7714

B1822+00 0.77895 0.876Ex15 276.3137 0.0721 30 243 95.4313 x0.5388 0.9982

B1822+00 0.77895 0.876Ex15 276.3137 0.0721 30 545 96.3183 x0.9454 0.8732

B1823x11 2.09314 0.491Ex14 276.5225 x11.5288 30 552 96.3346 11.2334 0.3501

B1823x11 2.09314 0.491Ex14 276.5225 x11.5288 30 905 97.3042 10.9341 0.9823

J1828x1101 0.07205 0.148Ex13 277.0783 x11.0308 30 552 96.3346 11.2334 0.7708

J1828x1101 0.07205 0.148Ex13 277.0783 x11.0308 30 905 97.3042 10.9341 0.2457

B1826x17 0.30713 0.555Ex14 277.4296 x17.8511 30 890 97.2654 17.7456 0.1951

B1828x10 0.40504 0.600Ex13 277.6979 x10.9911 30 905 97.3042 10.9341 0.3979

J1830x1135 6.22155 0.477Ex13 277.5071 x11.5842 30 905 97.3042 10.9341 0.6811

J1832x0644 0.74430 0.371Ex13 278.1775 x6.7338 31 069 97.7962 5.8771 0.9377

B1831x03 0.68670 0.416Ex13 278.4246 x3.6512 31 083 97.8396 2.9113 0.9432

J1833x0559 0.48346 0.124Ex13 278.2816 x5.9840 31 069 97.7962 5.8771 0.4970

J1833x0559 0.48346 0.124Ex13 278.2816 x5.9840 31 246 98.3021 5.4632 0.5213

J1834x0602 0.48791 0.183Ex14 278.6579 x6.0343 31 069 97.7962 5.8771 0.8759

J1834x0602 0.48791 0.183Ex14 278.6579 x6.0343 31 246 98.3021 5.4632 0.6729

J1834x1710 0.35831 0.469Ex16 278.7225 x17.1681 31 435 98.8029 18.0654 0.9010

J1837x1837 0.61836 0.550Ex14 279.4758 x18.6169 31 435 98.8029 18.0654 0.8700

J1839x0321 0.23878 0.125Ex13 279.9062 x3.3529 31 849 99.8804 3.3198 0.0420

J1839x0402 0.52094 0.769Ex14 279.9625 x4.0402 31 849 99.8804 3.3198 0.7251

J1841x0345 0.20407 0.589Ex13 280.4108 x3.8118 31 849 99.8804 3.3198 0.7235

B1839x04 1.83994 0.509Ex15 280.6100 x3.9999 31 849 99.8804 3.3198 0.9975

J1844+00 0.46050 0.100E+01 281.0458 0.5833 32 270 101.0583 x0.9254 0.3423

W.H. Edmondson and I.R. Stevens250

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B1842+14 0.37546 0.187Ex14 281.2283 14.9039 32 076 100.5221 x15.2149 0.7717

B1842+14 0.37546 0.187Ex14 281.2283 14.9039 32 303 101.1663 x14.7284 0.1861

J1849+06 2.21900 0.100E+01 282.2792 6.1167 32 524 101.8058 x5.6138 0.6906

J1849+24 0.27500 0.100E+01 282.2500 24.0000 32 662 102.1979 x23.2031 0.7986

J1850+0026 1.08184 0.359Ex15 282.6879 0.4404 32 608 102.0479 0.3049 0.9824

B1848+04 0.28470 0.109Ex14 282.7633 4.3033 32 644 102.1488 x4.0757 0.6554

B1848+04 0.28470 0.109Ex14 282.7633 4.3033 32 984 103.0763 x5.1737 0.9249

J1852x2610 0.33634 0.877Ex16 283.2475 x26.1702 32 874 102.7517 25.7608 0.6430

J1852x2610 0.33634 0.877Ex16 283.2475 x26.1702 33 277 103.8275 25.3756 0.9838

J1852x2610 0.33634 0.877Ex16 283.2475 x26.1702 33 356 104.0658 25.9598 0.8450

J1853+0545 0.12640 0.611Ex15 283.4933 5.7653 32 984 103.0763 x5.1737 0.7239

J1857+0526 0.34995 0.693Ex14 284.3159 5.4413 33 719 105.0754 x5.3674 0.7632

B1855+09 0.00536 0.178Ex19 284.4013 9.7215 33 109 103.4367 x9.5154 0.9864

B1851x79 1.27919 0.186Ex14 285.1017 x79.8634 33 932 105.6187 79.1646 0.8693

J1901+1306 1.83086 0.131Ex15 285.4529 13.1134 33 973 105.7292 x13.2179 0.2953

J1901x0906 1.78193 0.164Ex14 285.4708 x9.1030 33 995 105.8038 9.0237 0.3423

B1900+05 0.74658 0.129Ex13 285.6775 5.9405 33 719 105.0754 x5.3674 0.8313

B1900+01 0.72930 0.403Ex14 285.8746 1.5940 34 239 106.4696 x1.0200 0.8267

J1903+2225 0.65118 0.445Ex15 285.9704 22.4201 33 799 105.2688 x21.9648 0.8364

B1900x06 0.43189 0.340Ex14 285.9079 x6.5394 33 848 105.3979 6.9268 0.6404

B1901+10 1.85657 0.276Ex15 286.0100 10.1929 34 104 106.0737 x10.5068 0.3203

J1906+0912 0.77535 0.132Ex15 286.6183 9.2157 34 423 107.0392 x9.9688 0.8627

J1907+0918 0.22611 0.943Ex13 286.8433 9.3085 34 423 107.0392 x9.9688 0.6887

J1907+0919 5.16892 0.778Ex10 286.8096 9.3223 34 423 107.0392 x9.9688 0.6861

B1905+39 1.23576 0.541Ex15 286.8942 40.0349 34 254 106.5096 x39.8672 0.4196

J1908+0909 0.33656 0.349Ex13 287.0309 9.1534 34 423 107.0392 x9.9688 0.8154

B1906+09 0.83027 0.980Ex16 287.2446 9.2671 34 423 107.0392 x9.9688 0.7312

B1907+02 0.98983 0.553Ex14 287.4096 2.9141 34 848 108.1758 x3.1779 0.8104

J1909+0912 0.22295 0.358Ex13 287.3329 9.2149 34 423 107.0392 x9.9688 0.8091

B1907+12 1.44174 0.823Ex14 287.5562 12.5278 34 710 107.8238 x12.0412 0.5553

B1907x03 0.50460 0.219Ex14 287.6233 x3.1650 34 341 106.7888 3.4481 0.8813

J1910x5959A 0.00327 0.307Ex20 287.9279 x59.9741 34 804 108.0712 59.2652 0.7233

J1910x5959B 0.00836 x0.799Ex18 287.7166 x59.9836 34 804 108.0712 59.2652 0.8011

J1910x5959C 0.00528 0.220Ex20 287.7729 x60.0166 34 804 108.0712 59.2652 0.8085

J1910x5959D 0.00903 0.963Ex18 287.7183 x59.9848 34 804 108.0712 59.2652 0.8015

J1910x5959E 0.00457 x0.437Ex18 287.7171 x59.9839 34 804 108.0712 59.2652 0.8012

J1911x1114 0.00363 0.142Ex19 287.9550 x11.2395 34 767 107.9629 10.5122 0.7274

J1912+2525 0.62198 0.225Ex15 288.0775 25.4172 34 785 108.0200 x24.8921 0.5283

J1913+1145 0.30607 0.502Ex14 288.4325 11.7592 34 710 107.8238 x12.0412 0.6709

B1911+11 0.60100 0.656Ex15 288.5421 11.3677 34 710 107.8238 x12.0412 0.9847

J1918+08 2.12966 0.100E+01 289.6333 8.6342 35 642 110.3196 x8.8776 0.7281

B1918+19 0.82104 0.896Ex15 290.2658 19.8124 35 555 110.0538 x19.8187 0.2122

B1918+19 0.82104 0.896Ex15 290.2658 19.8124 35 851 110.8717 x20.0226 0.6412

B1919+20 0.76068 0.500Ex16 290.4646 20.0558 35 555 110.0538 x19.8187 0.4743

B1919+20 0.76068 0.500Ex16 290.4646 20.0558 35 851 110.8717 x20.0226 0.4084

B1920+20 1.17276 0.649Ex15 290.5333 20.2992 35 555 110.0538 x19.8187 0.6789

B1920+20 1.17276 0.649Ex15 290.5333 20.2992 35 851 110.8717 x20.0226 0.4371

B1920+21 1.07792 0.818Ex14 290.7229 21.1783 36 058 111.4708 x21.5832 0.8505

B1921+17 0.54721 0.430Ex16 290.7825 17.1026 35 741 110.5854 x17.8123 0.7365

B1921+17 0.54721 0.430Ex16 290.7825 17.1026 35 943 111.1425 x17.8921 0.8677

B1922+20 0.23779 0.209Ex14 291.1667 20.6667 35 851 110.8717 x20.0226 0.7085

B1922+20 0.23779 0.209Ex14 291.1667 20.6667 36 058 111.4708 x21.5832 0.9656

B1923+04 1.07408 0.246Ex14 291.6017 4.5254 35 881 110.9654 x5.2714 0.9804

B1924+16 0.57982 0.180Ex13 291.6887 16.8091 36 392 112.3346 x17.3449 0.8392

B1924+19 1.34601 0.143Ex14 291.5950 19.4699 35 851 110.8717 x20.0226 0.9103

B1929+15 0.31435 0.501Ex14 292.9821 15.6160 36 512 112.6662 x15.9943 0.4929

B1929+15 0.31435 0.501Ex14 292.9821 15.6160 36 809 113.5550 x16.1881 0.8097

B1929+20 0.26822 0.422Ex14 293.0333 20.3462 36 951 113.9492 x20.0484 0.9631

B1930+22 0.14447 0.576Ex13 293.0946 22.3476 36 731 113.3179 x22.3009 0.2282

J1932x3655 0.57142 0.284Ex15 293.0254 x36.9173 36 627 112.9896 36.2304 0.6877

J1933+07 0.43745 0.100E+01 293.3333 7.8833 36 587 112.8767 x8.1436 0.5256

B1931+24 0.81369 0.811Ex14 293.4075 24.6110 36 667 113.1571 x24.5728 0.2533

B1931+24 0.81369 0.811Ex14 293.4075 24.6110 37 109 114.3833 x24.5969 0.9759

Utilization of pulsars 251

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

B1933+16 0.35874 0.600Ex14 293.9492 16.2778 36 809 113.5550 x16.1881 0.4042

B1933+17 0.65441 0.378Ex15 293.8746 17.7534 36 901 113.8008 x17.5486 0.2177

B1933+15 0.96734 0.404Ex14 294.0063 15.6100 36 809 113.5550 x16.1881 0.7334

B1935+25 0.20098 0.643Ex15 294.2550 25.7371 37 309 114.8971 x26.4743 0.9776

J1938+06 1.12156 0.100E+01 294.5000 6.8667 37 413 115.2162 x7.2919 0.8330

B1937+21 0.00156 0.105Ex18 294.9104 21.5831 37 217 114.6692 x21.2234 0.4331

B1937+24 0.64530 0.183Ex13 294.7729 24.7154 37 109 114.3833 x24.5969 0.4072

B1941x17 0.84116 0.986Ex15 296.0217 x17.8336 37 622 115.7988 18.1796 0.4115

B1941x17 0.84116 0.986Ex15 296.0217 x17.8336 37 922 116.5683 17.0143 0.9850

B1943+18 1.06871 0.242Ex15 296.4004 18.5723 37 528 115.5379 x18.8291 0.8999

B1942x00 1.04563 0.535Ex15 296.3679 x0.6828 37 885 116.4704 0.8231 0.1738

B1944+22 1.33445 0.889Ex15 296.6033 22.7498 37 906 116.5150 x23.1416 0.4016

J1946+2611 0.43506 0.220Ex13 296.6908 26.1970 37 968 116.7379 x25.3704 0.8279

J1947+10 1.11094 0.100E+01 296.9000 10.7333 37 844 116.3717 x10.1607 0.7792

J1947+10 1.11094 0.100E+01 296.9000 10.7333 37 972 116.7487 x10.7574 0.1531

B1946x25 0.95762 0.327Ex14 297.3558 x25.4002 38 172 117.3288 24.4888 0.9119

B1946x25 0.95762 0.327Ex14 297.3558 x25.4002 38 312 117.7400 25.1107 0.4811

J1951+1123 5.09408 0.303Ex14 297.7842 11.3903 38 392 117.9829 x11.0326 0.4093

J1953+1149 0.85189 0.287Ex14 298.4475 11.8285 38 392 117.9829 x11.0326 0.9216

B1953+50 0.51894 0.137Ex14 298.8279 50.9987 38 649 118.7054 x50.5644 0.4512

B1953+50 0.51894 0.137Ex14 298.8279 50.9987 38 715 118.8942 x50.7090 0.2972

J2002+1637 0.27650 0.225Ex15 300.6988 16.6213 39 293 120.5150 x17.1722 0.5807

J2002+30 0.42179 0.100E+01 300.7417 30.5833 39 101 119.9879 x30.3756 0.7818

J2002+30 0.42179 0.100E+01 300.7417 30.5833 39 327 120.6104 x30.4180 0.2111

B2000+40 0.90507 0.174Ex14 300.6833 40.8483 39 007 119.7442 x40.9010 0.9406

B2002+31 2.11126 0.746Ex13 301.2175 31.6194 39 748 121.8558 x32.0091 0.7479

J2005x0020 2.27966 0.257Ex13 301.4321 x0.3394 39 669 121.5933 x0.1128 0.4800

B2003x08 0.58087 0.460Ex16 301.5679 x8.1172 39 721 121.7875 7.3837 0.7656

J2015+2524 2.30330 0.510Ex15 303.8029 25.4087 40 652 124.4775 x25.3612 0.6763

B2016+28 0.55795 0.148Ex15 304.5158 28.6651 40 424 123.8113 x28.6860 0.7049

B2016+28 0.55795 0.148Ex15 304.5158 28.6651 40 914 125.2504 x28.6249 0.7357

B2020+28 0.34340 0.189Ex14 305.6542 28.9064 40 914 125.2504 x28.6249 0.4922

B2022+50 0.37262 0.251Ex14 305.9246 50.6263 40 840 125.0096 x50.8837 0.9505

J2033+17 0.00595 0.110Ex19 308.3375 17.6000 42 281 129.3150 x17.4948 0.9832

J2038x3816 1.57729 0.413Ex14 309.7254 x38.2700 42 405 129.6971 38.1719 0.1020

J2038x3816 1.57729 0.413Ex14 309.7254 x38.2700 42 445 129.8125 37.5277 0.7474

J2040+16 0.86560 0.100E+01 310.0541 16.9000 42 281 129.3150 x17.4948 0.9487

J2040+16 0.86560 0.100E+01 310.0541 16.9000 42 844 130.9579 x17.0202 0.9117

J2043+2740 0.09613 0.127Ex14 310.9312 27.6682 42 872 131.0450 x28.1931 0.5370

J2044+4614 1.39271 0.630Ex15 311.2450 46.2348 42 847 130.9692 x46.4995 0.3823

B2044+15 1.13829 0.182Ex15 311.6637 15.6760 42 935 131.2696 x15.4246 0.4675

B2045+56 0.47673 0.111Ex13 311.6942 57.1436 42 885 131.0996 x57.7693 0.8632

B2043x04 1.54694 0.147Ex14 311.5004 x4.3572 42 862 131.0150 4.6415 0.5625

B2043x04 1.54694 0.147Ex14 311.5004 x4.3572 43 070 131.5954 4.5017 0.1729

B2045x16 1.96157 0.110Ex13 312.1475 x16.2790 43 217 132.0625 15.7276 0.5579

J2050+13 1.22000 0.100E+01 312.5000 13.0167 43 565 133.0850 x12.8084 0.6210

J2051x0827 0.00451 0.127Ex19 312.7812 x8.4605 43 618 133.2563 9.1858 0.8670

J2051x0827 0.00451 0.127Ex19 312.7812 x8.4605 43 692 133.4908 8.4215 0.7106

B2053+21 0.81518 0.134Ex14 313.9129 22.1576 43 921 134.2075 x22.5251 0.4710

B2053+36 0.22151 0.369Ex15 313.8804 36.5059 43 880 134.0829 x37.1225 0.6489

B2106+44 0.41487 0.862Ex16 317.0850 44.6969 45 072 137.7100 x45.3088 0.8747

J2108x3429 1.42310 0.350Ex14 317.1266 x34.4939 44 559 136.1871 34.4011 0.9441

J2108x3429 1.42310 0.350Ex14 317.1266 x34.4939 45 053 137.6400 34.6113 0.5266

B2110+27 1.20285 0.262Ex14 318.2679 27.9006 45 301 138.4979 x27.5198 0.4449

J2124x3358 0.00493 0.205Ex19 321.1825 x33.9789 46 022 140.7904 33.9056 0.3989

J2124x3358 0.00493 0.205Ex19 321.1825 x33.9789 46 098 141.0100 34.7969 0.8359

J2139+2242 1.08351 0.142Ex14 324.8621 22.7117 47 156 144.1354 x22.4297 0.7794

J2139+2242 1.08351 0.142Ex14 324.8621 22.7117 47 353 144.7287 x22.9649 0.2862

J2144x3933 8.50983 0.496Ex15 326.0504 x39.5653 47 527 145.3408 38.9505 0.9389

J2144x3933 8.50983 0.496Ex15 326.0504 x39.5653 47 581 145.5279 39.2473 0.6117

J2144x3933 8.50983 0.496Ex15 326.0504 x39.5653 47 933 146.5212 39.8710 0.5613

J2145x0750 0.01605 0.299Ex19 326.4600 x7.8384 47 587 145.5417 7.5901 0.9513

J2145x0750 0.01605 0.299Ex19 326.4600 x7.8384 47 722 145.9321 7.9531 0.5402

W.H. Edmondson and I.R. Stevens252

Table A1 (cont.)

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J2145x0750 0.01605 0.299Ex19 326.4600 x7.8384 48 165 147.2637 7.8193 0.8040

B2148+63 0.38014 0.168Ex15 327.4938 63.4954 48 018 146.8296 x63.7206 0.7013

B2148+63 0.38014 0.168Ex15 327.4938 63.4954 48 470 148.2608 x63.5129 0.7673

B2148+52 0.33221 0.101Ex13 327.6571 52.7971 48 133 147.1954 x52.6163 0.4958

B2148+52 0.33221 0.101Ex13 327.6571 52.7971 48 143 147.2167 x53.5854 0.9030

B2152x31 1.03000 0.124Ex14 328.8067 x31.3152 48 570 148.5950 32.2571 0.9654

B2152x31 1.03000 0.124Ex14 328.8067 x31.3152 48 740 149.1254 31.7388 0.5301

J2156+2618 0.49815 0.142Ex16 329.0988 26.3084 48 659 148.8496 x27.2609 0.9846

J2156+2618 0.49815 0.142Ex16 329.0988 26.3084 48 757 149.1721 x25.3372 0.9740

J2156+2618 0.49815 0.142Ex16 329.0988 26.3084 48 930 149.7350 x27.0659 0.9892

B2154+40 1.52527 0.343Ex14 329.2575 40.2961 48 718 149.0525 x40.7868 0.5318

J2205+1444 0.93801 0.900Ex15 331.3217 14.7420 49 577 151.8075 x14.3047 0.6537

B2210+29 1.00459 0.495Ex15 333.0971 29.5516 49 821 152.5571 x29.5048 0.5420

B2217+47 0.53847 0.277Ex14 334.9504 47.9150 50 436 154.4688 x48.3535 0.6514

B2217+47 0.53847 0.277Ex14 334.9504 47.9150 50 761 155.4846 x47.3591 0.7709

B2217+47 0.53847 0.277Ex14 334.9504 47.9150 50 866 155.7988 x48.3348 0.9465

J2222+2923 0.28140 0.617Ex17 335.7633 29.3996 50 568 154.9488 x28.9624 0.9245

J2222+2923 0.28140 0.617Ex17 335.7633 29.3996 50 681 155.2396 x28.7413 0.8413

J2222+2923 0.28140 0.617Ex17 335.7633 29.3996 50 807 155.5975 x28.8477 0.5763

J2222+2923 0.28140 0.617Ex17 335.7633 29.3996 50 921 155.9804 x29.6458 0.3282

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 297 157.1775 x27.3654 0.6936

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 494 157.7537 x26.8675 0.3217

J2229+2643 0.00298 0.146Ex20 337.4617 26.7327 51 657 158.3067 x26.8142 0.8489

J2229+6114 0.05162 0.783Ex13 337.2717 61.2359 51 166 156.7671 x62.0058 0.9205

J2229+6114 0.05162 0.783Ex13 337.2717 61.2359 51 177 156.7933 x62.0187 0.9173

B2227+61 0.44306 0.226Ex14 337.4242 62.0933 51 166 156.7671 x62.0058 0.6629

B2227+61 0.44306 0.226Ex14 337.4242 62.0933 51 177 156.7933 x62.0187 0.6353

J2248x0101 0.47723 0.659Ex15 342.1117 x1.0299 52 610 161.3717 1.0108 0.7403

J2253+1516 0.79224 0.665Ex16 343.3104 15.2772 52 990 162.6067 x15.1040 0.7247

J2253+1516 0.79224 0.665Ex16 343.3104 15.2772 53 250 163.3658 x15.8206 0.5463

B2255+58 0.36825 0.575Ex14 344.4904 59.1541 53 448 164.0046 x59.5223 0.6096

B2303+30 1.57589 0.289Ex14 346.4930 31.0005 54 400 166.9779 x30.1742 0.9580

B2303+30 1.57589 0.289Ex14 346.4930 31.0005 54 496 167.2400 x31.3274 0.8155

B2306+55 0.47507 0.199Ex15 347.0575 55.7933 54 187 166.2700 x56.4030 0.9959

B2306+55 0.47507 0.199Ex15 347.0575 55.7933 54 506 167.2721 x56.4339 0.6756

B2310+42 0.34943 0.112Ex15 348.2854 42.8869 54 984 168.8783 x42.6131 0.6531

J2317+1439 0.00344 0.242Ex20 349.2883 14.6587 55 066 169.0925 x14.6931 0.1988

B2323+63 1.43631 0.283Ex14 351.3054 63.2812 55 779 171.4312 x63.9723 0.7025

B2324+60 0.23365 0.353Ex15 351.7441 61.2268 55 691 171.1704 x61.6478 0.7116

B2327x20 1.64362 0.463Ex14 352.6117 x20.0916 56 399 173.4375 19.5627 0.9807

J2346x0609 1.18146 0.136Ex14 356.7100 x6.1665 57 369 176.4200 5.5001 0.7268

J2346x0609 1.18146 0.136Ex14 356.7100 x6.1665 57 676 177.4358 6.5235 0.8089

Utilization of pulsars 253

Table A2. 1066 c orrelations between pulsar positions and the habstar catalogue

Pulsar details Habstar details

Name P

spin

|dP/dt|RA Dec. Index RA Dec. Sep. (deg)

J0006+1834 0.69375 0.210Ex14 1.5200 18.5831 206 0.6467 18.8360 0.9092

J0006+1834 0.69375 0.210Ex14 1.5200 18.5831 493 1.4783 18.2354 0.3502

J0006+1834 0.69375 0.210Ex14 1.5200 18.5831 495 1.4813 18.0762 0.5083

B0011+47 1.24070 0.564Ex15 3.5738 47.7759 889 2.7329 48.1104 0.9049