J/MNRAS/417/114 HST/NICMOS Galactic Center survey catalogue (Dong+, 2011)
Hubble Space Telescope Paschen α survey of the Galactic Centre:
data reduction and products.
Dong H., Wang Q.D., Cotera A., Stolovy S., Morris M.R., Mauerhan J.,
Mills E.A., Schneider G., Calzetti D., Lang C.
<Mon. Not. R. Astron. Soc., 417, 114-135 (2011)>
=2011MNRAS.417..114D 2011MNRAS.417..114D
ADC_Keywords: Surveys ; Infrared sources ; Photometry, HST
Keywords: catalogues - surveys - stars: formation - Galaxy: centre -
infrared: stars
Abstract:
Our Hubble Space Telescope/Near-Infrared Camera and Multi-Object
Spectrometer (HST/NICMOS) Paschen α survey of the Galactic
Centre, first introduced by Wang et al. (2010MNRAS.402..895W 2010MNRAS.402..895W),
provides a uniform, panoramic, high-resolution map of stars and an
ionized diffuse gas in the central 416arcmin2 of the Galaxy. This
survey was carried out with 144 HST orbits using two narrow-band
filters at 1.87 and 1.90um in NICMOS Camera 3. In this paper, we
describe in detail the data reduction and mosaicking procedures
followed, including background level matching and astrometric
corrections. We have detected ∼570000 near-infrared (near-IR) sources
using the 'starfinder' software and are able to quantify photometric
uncertainties of the detections.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 145 570532 HST/NICMOS GC survey catalogue
table3.dat 93 152 Primary Paschen α emitting candidates
table4.dat 95 189 Secondary Paschen α emitting candidates
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- Seq [1/570532] Sequential number
8- 16 F9.5 deg RAdeg Right ascension in decimal degrees (J2000)
18- 26 F9.5 deg DEdeg Declination in decimal degrees (J2000)
28- 31 F4.2 arcsec e_RAdeg rms uncertainty on RA
33- 36 F4.2 arcsec e_DEdeg rms uncertainty on DE
38- 46 F9.5 deg GLON [0/360] Galactic Longitude
48- 55 F8.5 deg GLAT Galactic Latitude
59- 74 E16.11 uJy SF187N Flux of F187N (1.87 micron)
78- 93 E16.11 uJy SF190N Flux of F190N (1.90 micron)
97-112 E16.11 uJy e_SF187N rms uncertainty on SF187N
116-132 E17.11 uJy e_SF190N rms uncertainty on SF190N
133-136 F4.1 mag F187N Magnitude in F187N band (Vega system)
138-141 F4.1 mag F190N Magnitude in F190N band (Vega system)
143 I1 --- Nexp Total number of exposures covering
individual sources
145 I1 --- Qual [0/2] Quality flag, 0=best (1)
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Note (1): The quality flag as follows:
0 = Good
1 = Affected by bad pixel
2 = Could be faked sources near very bright sources due to local
electron fluctuation (see paper for details)
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Byte-by-byte Description of file: table[34].dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Sequential number, within the table
5- 13 F9.5 deg RAdeg Right ascension in decimal degrees (J2000.0)
15- 23 F9.5 deg DEdeg Declination in decimal degrees (J2000.0)
25- 28 F4.1 mag Hmag ? H magnitude from SIRIUS catalog (1)
29 A1 --- n_Hmag [a] a: Hmag from 2MASS
31- 34 F4.1 mag Kmag ? K magnitude from SIRIUS catalog (1)
35 A1 --- n_Kmag [a] a: Kmag from 2MASS
37- 40 F4.1 mag F190N F190N magnitude
42- 44 F3.1 --- r Flux ratio, f(1.87um)/f(1.90um)
46- 49 F4.2 --- Er Flux ratio excess (r-)
51- 54 F4.1 --- Ns Significance factor
56- 73 A18 --- Ctp Counterpart(s) (2)
75- 91 A17 --- Type Spectral type
93 A1 --- Loc [FQAC] Location (3)
95 I1 --- PI [0/3]? Problem index (only in table4) (4)
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Note (1): SIRIUS catalogue (Nishiyama et al. 2006ApJ...638..839N 2006ApJ...638..839N)
Note (2): The ground-based spectroscopically identified counterparts of our
Paschen α emitting sources and their types are from:
* Figer et al. (1999ApJ...514..202F 1999ApJ...514..202F, FQ_NNNW = qF NNNW
* Figer et al. (2002ApJ...581..258F 2002ApJ...581..258F, FA_NN = [FNG2002] NNN)
* Liermann et al. (2009, Cat. J/A+A/494/1137, Lie_NNN = LHO NNN)
* Martins et al. (2008A&A...478..219M 2008A&A...478..219M)
* Blum et al. (2001AJ....122.1875B 2001AJ....122.1875B, Blu01_NN = [BSP2001] NN)
* Cotera et al. (1999ApJ...510..747C 1999ApJ...510..747C, Cot_N)
* Homeier et al. (2003A&A...408..153H 2003A&A...408..153H, HoN = WR NNNaa)
* Muno et al. (2006ApJ...638..183M 2006ApJ...638..183M, Muno06_01)
* Mikles et al. (2006ApJ...651..408M 2006ApJ...651..408M, Mik06_01)
* Mauerhan et al. (2007ApJ...662..574M 2007ApJ...662..574M, M07_N)
* Mauerhan et al. (20010a, 2010ApJ...710..706M 2010ApJ...710..706M, Mau10a_NN)
* Mauerhan et al. (2010b, 2010ApJ...713L..33M 2010ApJ...713L..33M, Mau10b)
* Mauerhan et al. (2010c, 2010ApJ...725..188M 2010ApJ...725..188M, Mau10c_NN = [MCD2010] NN)
Note (3): Location as follows:
Q = source inside Quintuplet cluster
A = source inside Arches cluster
C = source inside Center cluster
F = source outside the clusters
Note (4): Problem index as follows:
1 = with the choice of Ns=4.5 (or 3.5), we label 30 (42) of the identified
Paschen α emitting candidates, since their total fluxes within
the central 5x5 pixel in the calibrated F190N images are reduced by
1%, compared with the images produced without "cosmic ray removal"
steps in the "drizzle" package (see Section 2.3).
2 = each of additional five (10) sources has a neighbour within 0.3arcsec
(i.e. ∼1FWHM of our PSF) and with a comparable flux (within a factor
of 10). The photometric accuracy of these candidates is somewhat
problematic.
3 = our visual examination removes another 10 sources, the photometry of
which is likely affected by the nearby bright sources
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Apr-2012