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Introduction to MIOSOTYS: A multiple-object, high-speed photometer


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MIOSOTYS is a multiple-object, high-speed photometer. It is currently operating on the 1.93m telescope at Observatoire de Haute-Provence (OHP), France. The instrument consists of a multi-fibre positioner which can access maximum 29 targets simultaneously, and an EMCCD camera which is capable of recording low-level light at high frame rate. This paper will describes the instrument's specifications as well as the performance, i.e., signal-to-noise ratio, under the current configuration (ProEM CCD + 1.93m telescope).
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Introduction to MIOSOTYS: a multiple-object, high-speed
I Chun Shih
, Alain Doressoundiram
, Yannick Boissel
, Fran¸coise Roques
, Frederic Dauny
Paul Felenbok
, Andree Fernandez
, Jean Guerin
, Hsiang Kuang Chang
, Chih-Yuan Liu
Institute o f Astronomy, National Tsing Hua University, Hsinchu, Taiwan;
LESIA, Observatoire de Paris, Meudon, France
MIOSOTYS is a multiple-object, high-speed photometer. It is currently operating on the 1.93m telescope at
Observatoire de Haute-Provence (OHP), France. The instrument consists of a multi-fibre positioner which can
access maximum 29 targets simultaneously, and an EMCCD camera which is capable of recording low-level light
at high frame rate. This pape r will describes the instrument’s specifications as well as the performance, i.e.,
signal-to-noise ratio, under the current configuration (ProEM CCD + 1.9 3m telescope).
Keywords: Instrumentation, MIOSOTYS, Time resolution, Imaging, Photometry
MIOSOTYS is ba sed on MEFOS (Meudon ESO Fibre Optical System) which is a multiple-fibre positioner and
was first designed for multi-objects spectro scopy, and was mounted on the 3.6-m ESO telescope at La Silla, Chile
in the 90’. It rema ins in excellent shape and, recently, has been re-commisioned by LESIA, Paris Observatory
to conduct high time resolution photometry. The instrument now consists of a multi-objects fibre system and
a high speed EMCCD camera. It has be implemented at the cassegrain focus of the 193 cm telescope at the
Observatoire de Haute-Provence (OHP), France
. The fibre positioner moves 29 arms to the targets within a
field of view of 25? arc-minute. Each arm is equipped with an individual viewing system for accura te setting
and carries one individual fibre that inter c ept 12? arc-sec on the sky. All the 29 fibre images are projected
onto a EMCCD camer a for fast photometry acquisition. Thus, the instrument will provide the observational
abilities for various astronomical researches, such as sur veying the small objects in Kuiper Belt, fast variability
in compact binaries, young stellar objects in star formation, etc.
Three technical observations have been carried in November 2 008, March and April 2009 at OHP. We have
test the newly designed mechanical interface, calibrated the instrument in this configuration with the existing
guiding system and bonette, and investigated the observation ability for future science operations. The science
observations begin in February 2010 with a dedicated high speed E MCCD camera which replac es the moder-
ate one used for technical evaluation. In this paper, we discuss the instrument’s properties and performance
measured in laboratory as well as in actual observation. This is to provide potential observers with a practical
guideline to plan their observation strategies.
The instrument consists of three parts: 30 fibre positioning arms fixed on a platform, an Acquisition a nd Guiding
Image System (AGIS) above the arm platform, and a CCD camera.
2.1 Arms and fibres
There are 30 positioning arms arranged in a c ircle of 200? mm diameter of at the edge of the field. One of the
arm (#1) is used solely for guiding sy stem, and r e st of 29 arms are for observing targets. Each arm s weeps a
triangular zone by 2 motions: translation by 130mm and rotation by ± 7 deg ree. The image fibre is fixed on
the arm tip which is electrically insulated. The image fibre is a glass fibre bundle of 900mm lo ng, the diameter
of the elementary fibre is 18µm. Its tra nsmission efficiency is about 40-45%. The viewing surface is 1.9×1.9mm.
The output end of the 29 image fibres are projected on to a CCD camera through the optics of AGIS with a
reduction factor.
2.2 EMCCD camera
We chose the ProEM
camera manufactured by Princeton Instr uments
as the imaging sensor for the instru-
ment. The sensor of e2v CCD201B is a back-illuminated, frame-transfer EMCCD with 1024×1024 image pixels
(or active area 13.3×1 3.3 mm). The large ima ge area c an cover all of 29 fibre images. The peak Q.E. at 530 nm
is 95%. The air cooling system maintains the operating temperature at -55
C or lower. At the temperature the
typical dark current is . 0 .008 electron/pixel/second. The re adout noise then depends on the readout modes:
electron-multiplying (EM) or low-noise (LN).
The EMCCD has dual readout amplifiers (or ports, see figure 1 ), one is a traditional series register for LN
mode. The other, for EM mode, is an extended multiplication register which provide 1 to 1000 times multipli-
cation which can be controlled in linear, absolute step. The dual ports design means that the camera can be
optimised to perform different type of observations. For example, EM mode is suitable for low-light, high speed
conditions, and LN mode is for more conventional observation (i.e., long exposure). The readout noise in EM
mode is significant greater (50 electro n rms at readout rate 10 MHz), but is effectively reduced to . 1 electron
rms when multiplicatio n gain is sufficiently applied (see section 3.2).
The CCD camera’s ability largely decides the performance of MIOSOTYS. This s e c tion describes some impor-
tant characteristics of the ProEM CC D camera, such as timing properties, and signa l-to-noise ratio. Other
components of the instrument and the telescope (O.H.P. 1.93 m) also play roles here.
3.1 Effective exposure time
Effective exposure time is restricted by CCD’s transferring and readout processes from imaging sens or to ADC
register output. By default, the ProEM camera operates at the “Frame Transfer” mode. Initially, the exposed
sensor receives incoming photons within a pre-programmed time (T
). Once the exp osure is finished, all the
electrons are shifted to an identica l, but masked sens or (see figure 1). It takes certain amount of time (readout
time, T
) for electrons in the masked sensor to be transferred through a readout register. During the transferring,
the emptied exposed sensor can immediately receive new photons. Thus it is very useful in applications which
require continuous imaging (100% duty cycle).
If T
< T
, however, one should be aware of that the exposed sensor has to wait for the electrons in the
masked se nsor to completely be read out. While in waiting, the exposed sensor still re mains open to the source.
Consequently, the actual e xposure time (T
) is effectively equal to T
. For example, the T
of a full 1024×1024
pixels image at readout rate of 10 MHz is 100 ms, thus one c an have time resolution which is at least equal to
or longer than T
Figure 1. Comparison of traditional CCD and ProEM EMCCD array structures. Credit: Princeton Instruments
Fortunately, ProEM camera provides observers several methods to reduce T
. O ne is to define sensor’s region
of interest (R.O.I.). The pixels outside the se le c ted regions will be skipped during the readout process, thus
reducing T
. In MIOSOTYS’ general operating mode, its 29 fibres are arranged into a 6 by 6 s quare matrix,
and the size of each fibre image projected on the CCD is 80 × 80 pixels (see figure 2 ). As a result, only an
area of 480 × 480 pixels are read out instead of 102 4 × 1024 pixels. Consequently, T
at the same readout rate
is reduced to . 60 ms. Second is to bin the pixels, i.e. 2×2, during the readout process, thus T
can further be
reduced. To achieve finer time resolution, one can combine fewer R.O.I. and/or binning configurations, as long
as the data quality is acceptable.
3.2 Signal-to-noise ratio
The signal-to -noise ratio (S/N) of a CCD is given by the well-known ”CCD equation” which ha s the form
S/N =
+ n
+ N
+ N
, (1)
where N
is the total (sky subtracted) number of photons from the source; n
is the number of pixels contained
within the software aperture; N
is the number of sky photons per pixel; N
is the dark current in elec trons
per pixel per second; and N
is the readout noise in electrons per pixel. In case the background and instrument
noises are low enough compared with N
, the S/N will approximately equal to
However, in the situatio n o f high time re solution photometry, the level of incoming photons from source may
be comparable to that of the instrument noises, so that the S/N deteriorates. The dark current, with sufficient
cooling and very short exposure time, is low enough to be ignored, therefore the readout noise becomes the
dominant noise factor term. Ever worse, the readout noise increa ses dramatically when readout rate goes faster.
Figure 2. (Left) Image of all 29 bres p rojected on the CCD sensor (1,024×1,024 pixels). (Right) Output of R.O.I., in
which the active size reduces to 480×480 pixels. The vertical lines are artificially added by data acquisition software, and
can be removed after bias correction.
3.2.1 Electron-multiplying technique
To amplify the signal (photoelectrons) from instrument background, the camera uses electron-multiplying ga in
technology. T he multiplication takes place in the ex tended multiplication register through a process called im-
pact ionisation. The process is to amplify the electrons before they reach the output amplifier and subsequent
electronics. This will effectively boost the signal above the readout noise of the system. The process can take as
many as stages which corresponds to one pixel in the register. The probability of multiplication per stage is p,
and the total effective gain, G, is related to the number of stages, N. This gain factor is then given by
G = (1 + p)
, (2)
The probability of multiplication in each stage is actually small, in the range of 1% to 1.5%; however, by passing
through large number of stage s, the total multiplication gain can be quite high. Reading image out through the
multiplication register introduces an additional noise term called excess noise factor (F ), thereby the S/N of an
EMCCD is given by
S/N =
× F
) + n
× F
) + (N
× F
) + (N
, (3)
where F is 1.4.
Applying a ppropriate amount of EM gain (G) effectively reduces the readout noise to below 1 electron.
However, the excess noise factor due to multiplicatio n proce ss also consequently reduces the S/N by the factor.
As a result, the advantage of EMCCD becomes appa rently only whenever it is operated in high-speed, low-light
situations. Because the number of incoming photons per frame is low, the penalty of F is not so significant (see
figure 3).
3.3 Transmission efficiency
Fibre images are projected onto the CCD sensor through a lens component (within AGIS), and it is realised
that the transmission efficiency varies depending on the light passing thro ugh different part of the lens: images
at centre have better transmissio n than that at the edge. To quantify the transmissio n efficiency, we measured
all 29 fibr e s individually using the same, stable light source. Table 1 lists the rela tive transmission efficiency
Figure 3. Simulation of CCD S/N relating to conventional and EM gain modes. Conventional (black solid line): traditional
readout register. I n ProEM camera, its fastest readout rate (5 MHz) is lower than that in EM gain register (10 MHz),
so that the S/N is higher. EM: 1 stage (red dashed line): the readout goes through EM register, but no gain is applied,
thereby readout noise is not suppressed, and its S/N is even worse. EM: 500 stages (red solid line): 500 stage gain is
applied in the register. The S/N begins to improve as source becomes fainter. The magnitude scale is derived from the
observation took place in March 2009.
compared to the fibre 28, and figure 4 shows the geometric distribution of the transmission efficiency. In cases if it
is possible observers are suggested to assign central fibres to fainter targets to achieve reasonable signal-to -noise
Table 1. Relative transmission efficiency by optical system.
Fibre eff. Fibre eff. Fibre eff. Fibre eff. Fibre eff.
28 1.00 22 0.89 24 0.79 1 8 0.63 25 0.53
30 0.98 1 5 0.86 10 0.76 11 0.62 3 0.48
16 0.96 2 9 0.83 12 0.76 21 0.61 13 0.45
8 0.94 7 0.81 27 0.70 5 0.58 20 0.45
9 0.92 17 0.81 6 0.67 4 0.55 26 0.40
23 0.91 2 0.80 14 0.66 19 0.53
3.4 O.H.P. 1.93m telescope
The telescope is the host for MIOSOTYS mission. Beca use the instrument typically operates at time scale of .
1s, it is clear that the signals from targets with magnitude & 12 will be overwhelmed by the readout noise if EM
gain is not applied. Based on recent observation, figure 5 shows the improvement on S/N using EM gain of 500
at time resolution of .0.1s. O ne can obtain acceptable S/N of several hundreds from targ e ts with magnitudes
Figure 4. The geometric distribution of transmission efficiency.
between 12.0 and 14.5. Furthermo re, it is worth to notice that increa sing EM gain would not improve S/N
linearly, the experience suggests that 500 is enough for our mission.
As discussed earlier, EM gain is only useful when the rec eived photon is lower than certain level. One has
to justify the use of E M gain by considering important parameters, such as time resolution, and target brightness.
We introduced MIOSOTYS, a multi-object, fast photometry instrument based on EMCCD camera. The instru-
ment is mounted on the 1.93m telescope at O.H.P. and maximum 29 ta rgets can be observed simultaneously
at time resolution of &50 ms . The electron-multiplying technology on the camera allows observers to access
fainter targets with higher time resolution. It opens a new door for temporal-related astronomical researches,
such as searching small Kuiper Belt objects, fast oscillation in compact objects and young stellar objects. We
also welcome and invite other observers to use this instrument.
This work is supported by the National Science Council (NSC), Taiwan with grants “NSC 96-2628-M-007-012-
MY3”, “NSC 98-2923-M-00 7-002-MY3”, and NSC 98-2811-M-007-001”, as well as by the Agence Nationale
pour la Recherche (ANR), France with grant “BLAN08- 2
328288” under the project of “Beyond Neptune”.
Figure 5. Comparison of S/N to different configurations of EM gain and exposure time. The results were derived from the
same group of stars and the same fibres were used. The magnitudes are quoted from the NOMAD catalogue. Observation
date: (circle) 01 March 2010; (square) 28 February 2010
1. L. Mortara and A. Fowler, Evaluations of charge-coupled device / ccd / performance for astronomical use,”
SOLID STATE IMAGERS FOR ASTRONOMY: SPIE#290 1981 P. 28 290, p. 28, Jan 1981.
2. D. Tody, “The iraf data reduction and analysis s ystem,” IN: Instrumentation in astronomy VI; Proceedings
of the Meeting 627, p. 733, Jan 19 86.
... Shih electron rms when sufficient multiplication gain is applied. For more information about the camera characteristics and experiment configuration, one should refer to [1] ...
... On the other hand, it is relatively easier to accumulate a huge data volume in optical bands, see, e.g., the Miosotys (Shih et al. 2010), TAOS II (Lehner et al. 2014) and CHIMERA (Harding et al. 2016) projects. Because of longer wavelength, however, it can probe objects only down to size of 1 km, 10 km and 30 km or so for the Kuiper Belt, inner and outer Oort Cloud, respectively, again due to diffraction limit. ...
Using all the RXTE archival data of Sco X-1 and GX 5-1, which amount to about 1.6 mega seconds in total, we searched for possible occultation events caused by Oort Cloud Objects. The detection efficiency of our searching approach was studied with simulation. Our search is sensitive to object size of about 300 m in the inner Oort Cloud, taking 4000 AU as a representative distance, and of 900 m in the outer Oort Cloud, taking 36000 AU as the representative distance. No occultation events were found in the 1.6 Ms data. We derived upper limits to the number of Oort Cloud Objects, which are about three orders of magnitude higher than the highest theoretical estimates in the literature for the inner Oort Cloud, and about six orders higher for the outer Oort Cloud. Although these upper limits are not constraining enough, they are the first obtained observationally, without making any model assumptions about comet injection. They also provide guidance to such serendipitous occultation event search in the future.
Full-text available
We report the effort to search for white dwarf p-mode oscillations in RX J2117.1+ 3412 (V2027 Cyg), a GW Vir star. The data were taken with Miosotys, a multi-fiber photometer, mounted on the 1.93-m telescope at Observatoire de Haute-Provence (OHP) with a 20-Hz cadence in May 2010 and June 2012. Two intriguing signatures at 1.2081 Hz and 2.5852 Hz were found at 3.8-s and 3.5-s significance levels, respectively. However, possible atmospheric effects cannot be ruled out. If these two features are not real, the 3-s upper limit of the relative amplitude for the possible oscillations in the frequency range from 1 to 10 Hz is estimated to be about 6 x 10-4. This is the first report in the literature for a p-mode oscillation search of GW Vir stars.
When CCD imaging arrays are used for astronomy the demands placed upon them are generally considerably different than those placed upon them in general TV applications. In both cases the parameters used to characterize a given array are generally the same but the target values for the parameters may vary significantly. The emphasis placed upon certain characteristics may also vary significantly depending on the particular application. Since, for some of the parameters at least, different methodologies provide different values it is important to understand how each value is obtained. It is the purpose of this paper to describe some of the methods used by one group at KPNO for determining the values of the primary parameters.
The iraf data reduction and analysis system
  • D Tody
D. Tody, "The iraf data reduction and analysis system," IN: Instrumentation in astronomy VI; Proceedings of the Meeting 627, p. 733, Jan 1986.