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M. J. Page,
C. Brindle,
A. Talavera,
M. Still,
S. R. Rosen,
V. N. Yershov,
H. Ziaeepour,
K. O. Mason,
M. S. Cropper,
A. A. Breeveld,
N. Loiseau,
R. Mignani, A. Smith,
P. Murdin
[show abstract]
[hide abstract]
ABSTRACT: The XMM-Newton Serendipitous Ultraviolet Source Survey (XMM-SUSS) is a
catalogue of ultraviolet (UV) sources detected serendipitously by the Optical
Monitor (XMM-OM) on-board the XMM-Newton observatory. The catalogue contains
ultraviolet-detected sources collected from 2,417 XMM-OM observations in 1-6
broad band UV and optical filters, made between 24 February 2000 and 29 March
2007. The primary contents of the catalogue are source positions, magnitudes
and fluxes in 1 to 6 passbands, and these are accompanied by profile
diagnostics and variability statistics. The XMM-SUSS is populated by 753,578 UV
source detections above a 3 sigma signal-to-noise threshold limit which relate
to 624,049 unique objects. Taking account of substantial overlaps between
observations, the net sky area covered is 29-54 square degrees, depending on UV
filter. The magnitude distributions peak at 20.2, 20.9 and 21.2 in UVW2, UVM2
and UVW1 respectively. More than 10 per cent of sources have been visited more
than once using the same filter during XMM-Newton operation, and > 20 per cent
of sources are observed more than once per filter during an individual visit.
Consequently, the scope for science based on temporal source variability on
timescales of hours to years is broad. By comparison with other astrophysical
catalogues we test the accuracy of the source measurements and define the
nature of the serendipitous UV XMM-OM source sample. The distributions of
source colours in the UV and optical filters are shown together with the
expected loci of stars and galaxies, and indicate that sources which are
detected in multiple UV bands are predominantly star-forming galaxies and stars
of type G or earlier.
07/2012;
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K. Mitchell-Wynne,
A. Cooray,
Y. Gong,
M. Bethermin,
J. Bock,
A. Franceschini,
J. Glenn,
M. Griffin,
M. Halpern,
L. Marchetti, [......],
I. Perez-Fournon,
B. Schulz,
D. Scott,
J. Smidt, A. Smith,
M. Vaccari,
L. Vigroux,
L. Wang,
J. L. Wardlow,
M. Zemcov
[show abstract]
[hide abstract]
ABSTRACT: The wide-area imaging surveys with the {\it Herschel} Space Observatory at
sub-mm wavelengths have now resulted in catalogs of order one hundred thousand
dusty, star-burst galaxies. We make a statistical estimate of $N(z)$ using a
clustering analysis of sub-mm galaxies detected at each of 250, 350 and 500
$\mu$m from the Herschel Multi-tiered Extragalactic Survey (HerMES) centered on
the Bo\"{o}tes field. We cross-correlate {\it Herschel} galaxies against galaxy
samples at optical and near-IR wavelengths from the Sloan Digital Sky Survey
(SDSS), the NOAO Deep Wide Field Survey (NDWFS) and the Spitzer Deep Wide Field
Survey (SDWFS). We create optical and near-IR galaxy samples based on their
photometric or spectroscopic redshift distributions and test the accuracy of
those redshift distributions with similar galaxy samples defined with catalogs
of the Cosmological Evolution Survey (COSMOS), as the COSMOS field has superior
spectroscopy coverage. We model-fit the clustering auto and cross-correlations
of {\it Herschel} and optical/IR galaxy samples to estimate $N(z)$ and
clustering bias factors. The $S_{350} > 20$ mJy galaxies have a bias factor
varying with redshift as $b(z)=1.0^{+1.0}_{-0.5}(1+z)^{1.2^{+0.3}_{-0.7}}$.
This bias and the redshift dependence is broadly in agreement with galaxies
that occupy dark matter halos of mass in the range of 10$^{12}$ to 10$^{13}$
M$_{\sun}$. We find that the redshift distribution peaks around $z \sim 0.5$ to
1 for galaxies selected at 250 $\mu$m with an average redshift of $< z > = 1.8
\pm 0.2$. For 350 and 500 $\mu$m-selected SPIRE samples the peak shifts to
higher redshift, but the average redshift remains the same with a value of $1.9
\pm 0.2$.
02/2012;
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K Tsumura,
T Arai,
J. Battle,
J. Bock,
S Brown,
A. Cooray,
V. Hristov,
B. Keating,
M. G. Kim,
D H Lee, [......],
T Matsumoto,
S Matsuura,
K Murata,
U. W. Nam,
T. Renbarger, A Smith,
I. Sullivan,
K Suzuki,
T Wada,
M. Zemcov
[show abstract]
[hide abstract]
ABSTRACT: Absolute spectrophotometric measurements of diffuse radiation at 1 \mu m to 2
\mu m are crucial to our understanding of the radiative content of the Universe
from nucleosynthesis since the epoch of reionization, the composition and
structure of the Zodiacal dust cloud in our solar system, and the diffuse
galactic light arising from starlight scattered by interstellar dust. The Low
Resolution Spectrometer (LRS) on the rocket-borne Cosmic Infrared Background
Experiment (CIBER) is a \lambda / \Delta \lambda \sim 15-30 absolute
spectrophotometer designed to make precision measurements of the absolute
near-infrared sky brightness between 0.75 \mu m < \lambda < 2.1 \mu m. This
paper presents the optical, mechanical and electronic design of the LRS, as
well as the ground testing, characterization and calibration measurements
undertaken before flight to verify its performance. The LRS is shown to work to
specifications, achieving the necessary optical and sensitivity performance. We
describe our understanding and control of sources of systematic error for
absolute photometry of the near-infrared extragalactic background light.
12/2011;
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G. Tinetti,
J. P. Beaulieu,
T. Henning,
M Meyer,
G. Micela,
I. Ribas,
D. Stam,
M. Swain,
O. Krause,
M. Ollivier, [......],
G. Vasisht,
S. Vinatier,
S. Viti,
I. Waldmann,
G. J. White,
T Widemann,
R. Wordsworth,
R. Yelle,
Y. Yung,
S. N. Yurchenko
[show abstract]
[hide abstract]
ABSTRACT: A dedicated mission to investigate exoplanetary atmospheres represents a
major milestone in our quest to understand our place in the universe by placing
our Solar System in context and by addressing the suitability of planets for
the presence of life. EChO -the Exoplanet Characterisation Observatory- is a
mission concept specifically geared for this purpose. EChO will provide
simultaneous, multi-wavelength spectroscopic observations on a stable platform
that will allow very long exposures. EChO will build on observations by Hubble,
Spitzer and groundbased telescopes, which discovered the first molecules and
atoms in exoplanetary atmospheres. EChO will simultaneously observe a broad
enough spectral region -from the visible to the mid-IR- to constrain from one
single spectrum the temperature structure of the atmosphere and the abundances
of the major molecular species. The spectral range and resolution are tailored
to separate bands belonging to up to 30 molecules to retrieve the composition
and temperature structure of planetary atmospheres. The target list for EChO
includes planets ranging from Jupiter-sized with equilibrium temperatures Teq
up to 2000 K, to those of a few Earth masses, with Teq ~300 K. We have
baselined a dispersive spectrograph design covering continuously the 0.4-16
micron spectral range in 6 channels (1 in the VIS, 5 in the IR), which allows
the spectral resolution to be adapted from several tens to several hundreds,
depending on the target brightness. The instrument will be mounted behind a 1.5
m class telescope, passively cooled to 50 K, with the instrument structure and
optics passively cooled to ~45 K. EChO will be placed in a grand halo orbit
around L2. We have also undertaken a first-order cost and development plan
analysis and find that EChO is easily compatible with the ESA M-class mission
framework.
12/2011;
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M. J. Griffin,
A. Abergel,
A. Abreu,
P. A. R. Ade,
P. André,
J. L. Augueres,
T. Babbedge,
Y. Bae,
T. Baillie,
J.-P. Baluteau, [......],
N. Whitehouse,
C. D. Wilson,
B. Winter,
A. L. Woodcraft,
G. S. Wright,
C. K. Xu,
A. Zavagno,
M. Zemcov,
L Zhang,
E. Zonca
[show abstract]
[hide abstract]
ABSTRACT: The Spectral and Photometric Imaging Receiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 microns, and an imaging Fourier Transform Spectrometer (FTS) which covers simultaneously its whole operating range of 194-671 microns (447-1550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4' x 8', observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6'. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5-2. Comment: Accepted for publication in Astronomy & Astrophyics (Herschel first results special issue)
05/2010;
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J Fischer,
L ~M Shier,
M ~L Luhman,
S Satyapal,
H ~A Smith,
G ~J Stacey,
S ~J Unger,
M ~A Greenhouse,
L Spinoglio,
M ~A Malkan, [......],
T Lim,
S Molinari,
Nguyen-Q-Rieu,
M ~C Price,
S ~D Sidher, A Smith,
B ~M Swinyard,
D Texier,
N ~R Trams,
M ~G Wolfire
Revista Mexicana de Astronomia y Astrofisica Conference Series; 05/1997
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R. Emery,
P Aannestad,
N Minchin,
S. J. Unger,
J.-P. Baluteau,
M. J. Barlow,
E. Caux,
G. Serra,
M Joubert,
D. Lorenzetti, [......],
D Texier,
S D Sidher,
N Trams,
B. Swinyard,
K King,
H Smith,
I Furniss,
D Ewart,
M Price, A Smith
[show abstract]
[hide abstract]
ABSTRACT: Grating spectra, covering the wavelength range 45 to 187μm have been
taken with the ISO Long Wavelength Spectrometer (LWS) at a series of
pointing positions over the S 140 region, centred on the cluster of
embedded young stellar objects at the south-west corner of the L1204
molecular cloud. Extended emission from [CII]158μm and [OI]63μm is
seen, peaking near the position of the embedded stars. The measurements
of the fine structure lines are interpreted in terms of PDR models for
the emission, as well as the underlying thermal continuum for the heated
gas and dust.
Astronomy and Astrophysics 10/1996; · 4.59 Impact Factor
-
R. Emery,
P Aannestad,
N Minchin,
S. J. Unger,
J.-P. Baluteau,
M. J. Barlow,
E. Caux,
G. Serra,
M Joubert,
D. Lorenzetti, [......],
D Texier,
S D Sidher,
N Trams,
B. Swinyard,
K King,
H Smith,
I Furniss,
D Ewart,
M Price, A Smith
-
MJ Griffin,
DA Naylor,
GR Davis,
PAR Ade,
PG Oldham,
BM Swinyard,
D. Gautier,
E. Lellouch,
GS Orton,
T. Encrenaz, [......],
KJ King,
T Lim,
S. Molinari,
M Price,
S. Sidher, A Smith,
D Texier,
N Trams,
SJ Unger,
A Salama
-
GR Davis,
MJ Griffin,
DA Naylor,
PG Oldham,
BM Swinyard,
PAR Ade,
SB Calcutt,
T. Encrenaz,
T DeGraauw,
D. Gautier, [......],
C. Gry,
KJ King,
T Lim,
S. Molinari,
M Price,
S. Sidher, A Smith,
D Texier,
N Tran,
SJ Unger
-
J Fischer,
LM Shier,
ML Luhman,
S. Satyapal,
HA Smith,
GJ Stacey,
SJ Unger,
MA Greenhouse,
L. Spinoglio,
MA Malkan, [......],
T Lim,
S. Molinari,
Q NguyenRieu,
MC Price,
SD Sidher, A Smith,
BM Swinyard,
D Texier,
NR Trams,
MG Wolfire
-
Article:
The
M. J. Griffin,
A. Abergel,
A. Abreu,
P. A. R. Ade,
P. André,
J. L. Augueres,
T. Babbedge,
Y. Bae,
T. Baillie,
J.-P. Baluteau, [......],
N. Whitehouse,
C. D. Wilson,
B. Winter,
A. L. Woodcraft,
G. S. Wright,
C. K. Xu,
A. Zavagno,
M. Zemcov,
L Zhang,
E. Zonca
http://dx.doi.org/10.1051/0004-6361/201014519.
