J/other/RAA/19.29 Compilation of known QSOs for the Gaia mission (Liao+, 2019)
A compilation of known QSOs for the Gaia mission.
Liao S.-L., Qi Z.-x., Guo S.-f., Cao Z.-h.
<Res. Astron. Astrophys., 19, 29 (2019)>
=2019RAA....19...29L 2019RAA....19...29L (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Photometry, SDSS ; Photometry, infrared ; Redshifts
Keywords: astrometry - catalogs - quasars - astrometric - parallax bias -
Gaia catalog
Abstract:
Quasars are essential for astrometric in the sense that they are
spatial stationary because of their large distance from the Sun. The
European Space Agency (ESA) space astrometric satellite Gaia is
scanning the whole sky with unprecedented accuracy up to a few uas
level. However, Gaia's two fields of view observations strategy may
introduce a parallax bias in the Gaia catalog. Since it presents no
significant parallax, quasar is perfect nature object to detect such
bias. More importantly, quasars can be used to construct a Celestial
Reference Frame in the optical wavelengths in Gaia mission. In this
paper, we compile the most reliable quasars existing in
literatures.The final compilation (designated as Known Quasars Catalog
for Gaia mission, KQCG) contains 1842076 objects, among of them,
797632 objects are found in Gaia DR1 after cross-identifications. This
catalog will be very useful in Gaia mission.
Description:
KQCG (Known QSOs catalog for Gaia mission) is a compilation of quasars
from LQAC3, SDSS DRQ14, LAMOST DR5 and MIRAGNs from AllWISE. This
catalog convers the whole sky, and contains 1842076 objects. KQCG can
be used in the Gaia mission in the following three aspects: 1) They
can be selected to build the Gaia celestial reference frame. With such
a large number of QSOs and uniform spatial distribution, one can
statistics analysis the overall properties of this new Celestial
Reference Frame with respect to their spatial distribution, accuracy,
magnitude distribution. 2). As the parallaxes and the proper motions
of the QSOs can be treated as zero, they can be used to detect the
parallax bias of the Gaia catalog and as additional quality indicators
to evaluate the overall quality of the Gaia catalog. 3). A comparison
of those QSOs in radio wavelength with optical counterparts can be
made between the Gaia solution and the VLBI solution. More
importantly, these QSOs in radio wavelength with optical counterparts
can be used to link the ICRF between the radio and optical band.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
kqcg.dat 203 1842076 Known QSOs catalog for Gaia mission catalog
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
II/328 : AllWISE Data Release (Cutri+ 2013)
J/A+A/583/A75 : Large Quasar Astrometric Catalog 3 (LQAC-3) (Souchay+, 2015)
Byte-by-byte Description of file: kqcg.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Name (1)
25- 38 E14.10 deg RAdeg Right ascension (J2000.0) (2)
40- 53 E14.10 deg DEdeg Declination (J2000.0) (2)
55- 75 E21.17 arcsec e_RAdeg ? Error in Right ascension
77- 97 E21.17 arcsec e_DEdeg ? Error in Declination
99-111 F13.10 --- z ? Redshift (3)
113-123 F11.8 mag umag ? u photographic magnitude (4)
125-135 F11.8 mag gmag ? g photographic magnitude (4)
137-147 F11.8 mag rmag ? r photographic magnitude (4)
149-159 F11.8 mag imag ? i photographic magnitude (4)
161-171 F11.8 mag zmag ? z photographic magnitude (4)
173-187 A15 --- Ref Reference catalog (5)
189-192 F4.2 mag W1-W2 ? W1-W2 photographic magnitude (6)
194-197 F4.2 mag W2-W3 ? W2-W3 photographic magnitude (6)
199-203 F5.2 mag W1mag ? W1 photographic magnitude (6)
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Note (1): The reference name of the quasar in the catalog. If there is a name
from its origin catalog, the original name is used. Otherwise, it will be
designated by its equatorial coordinates calculated in degree and truncated
to the arcsecond level.
Note (2): The equatorial coordinates (alpha,delta) of the object given by the
original catalog.
Note (3): The redshift value z of each quasar. The value comes from its
original catalog, and will be set empty if no redshift is provided.
Note (4): The apparent magnitudes in the u, g, r, i, z bands, respectively.
These photometric values come from their origin catalogs. When the magnitude
is not available, the value will be set empty.
Note (5): The reference catalog or flag indicating the presence of the quasar
in one of the 12 catalogs from A to P:
A = ICRF2
B = VLBA
C = VLA
D = JVAS
E = SDSS
F = 2QZ
G = 2df-SDSS LRG
H = FIRST
I = HB
M = V&V
O = LAMOST
P = MIRAGNs
Q = Gaia DR1
Also see J/A+A/583/A75 : Large Quasar Astrometric Catalog 3 (LQAC-3)
(Souchay+, 2015).
Note (6): The W1, W2 and W3 magnitude information of the sources from MIRAGNs.
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History:
From Shilong Liao, shilongliao(at)shao.ac.cn
Acknowledgements:
This work has made use of data from the European Space Agency (ESA)
mission Gaia,processed by the Gaia Data Processing and Analysis
Consortium (DPAC). This publication makes use of data products from
the Wide-field Infrared Survey Explorer, which is a joint project of
the University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration. Guoshoujing Telescope (the Large
Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a
National Major Scientific Project built by the Chinese Academy of
Sciences. Funding for the project has been provided by the National
Development and Reform Commission. LAMOST is operated and managed by
the National Astronomical Observatories, Chinese Academy of Sciences.
This work has been supported by the grants from the National Science
Foundation of China (NSFC) through grants 11703065 and 11573054.
(End) Shilong Liao [SHAO, China], Patricia Vannier [CDS] 18-Jan-2019