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J/ApJ/675/491       Lynds 988e JHKs and IRAC photometry      (Allen+, 2008)

Spitzer, near-infrared, and submillimeter imaging of the relatively sparse young cluster, Lynds 988e. Allen T.S., Pipher J.L., Gutermuth R.A., Megeath S.T., Adams J.D., Herter T.L., Williams J.P., Goetz-Bixby J.A., Allen L.E., Myers P.C. <Astrophys. J., 675, 491-506 (2008)> =2008ApJ...675..491A
ADC_Keywords: Associations, stellar ; Stars, pre-main sequence ; Photometry, infrared ; Photometry, millimetric/submm Keywords: infrared: stars - stars: pre-main sequence - stars: formation Abstract: We present Spitzer images of the relatively sparse, low-luminosity young cluster L988e (NAME [C86] L988 e CLUSTER in Simbad), as well as complementary near-infrared (NIR) and submillimeter images of the region. Description: NIR images in the J, H, and Ks wave bands of L988e were first obtained by the authors on 2002 October 26 using the Simultaneous Quad Infrared Imaging Device (SQIID), which houses four 1024x1024 InSb arrays, of which only 512x512 are used, on the 2.1m telescope at the Kitt Peak National Observatory, a facility of the National Optical Astronomical Observatory. Higher spatial resolution, deep, NIR observations in the J (1.25um), H (1.65um), and Ks (2.15um) wave bands were obtained on 2004 July 6 with the Palomar Widefield IR Camera (WIRC), which houses a 2048x2048 HgCdTe array. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 153 19 *Objects with Mid-Infrared Excesses: Class I table3.dat 153 74 *Objects with Mid-Infrared Excesses: Class II table4.dat 153 7 *Objects with Mid-Infrared Excesses: Transition disks table5.dat 153 20 *Objects without Mid-Infrared Excesses: Class III
Note on table*.dat: Extragalactic Contaminants Removed. Sources identified as [APG2008] JHHMMSS.ss+DDMMSS.ss in Simbad.
See also: J/AJ/131/1530 : Hα emission stars in LDN988 (Herbig+, 2006) Byte-by-byte Description of file: table?.dat
Bytes Format Units Label Explanations
1- 2 I2 h RAh Right ascension (J2000.0) 4- 5 I2 min RAm Right ascension (J2000.0) 7- 11 F5.2 s RAs Right ascension (J2000.0) 13- 16 F4.2 s e_RAs rms uncertainty on RA 18 A1 --- DE- Declination sign (J2000.0) 19- 20 I2 deg DEd Declination (J2000.0) 22- 23 I2 arcmin DEm Declination (J2000.0) 25- 29 F5.2 arcsec DEs Declination (J2000.0) 31- 34 F4.2 arcsec e_DEs rms uncertainty on DE 36- 40 F5.2 mag Jmag ? Dereddened J magnitude (1) 42- 47 F6.3 mag e_Jmag ? rms uncertainty on Jmag 49- 53 F5.2 mag Hmag ? Dereddened H magnitude (1) 55- 59 F5.3 mag e_Hmag ? rms uncertainty on Hmag 61- 65 F5.2 mag Ksmag ? Dereddened Ks magnitude (1) 67- 71 F5.3 mag e_Ksmag ? rms uncertainty on Ksmag 73- 77 F5.2 mag [3.6] ? Dereddened 3.6 magnitude (1) 79- 83 F5.3 mag e_[3.6] ? rms uncertainty on [3.6] 85- 89 F5.2 mag [4.5] ? Dereddened 4.5um magnitude (1) 91- 95 F5.3 mag e_[4.5] ? rms uncertainty on [4.5] 97-101 F5.2 mag [5.8] ? Dereddened 5.8um magnitude (1) 103-107 F5.3 mag e_[5.8] ? rms uncertainty on [5.8] 109-113 F5.2 mag [8.0] ? Dereddened 8.0um magnitude (1) 115-119 F5.3 mag e_[8.0] ? rms uncertainty on [8.0] 121-124 F4.2 mag [24] ? Dereddened 24um magnitude (1) 126-130 F5.3 mag e_[24] ? rms uncertainty on [24] 132-135 F4.2 mag AKs ? Absoption in Ks band (2) 137-142 F6.3 --- alpha ? Slope α determined from IRAC photometry 143 A1 --- n_alpha [gf] how α is computed (3) 145-147 I3 --- IfAHA ? Herbig & Dahm (2006, Cat. J/AJ/131/1530) ID 149-153 F5.1 0.1nm EWHa ? Halpha equivalent width (4)
Note (1): Magnitudes are dereddened when extinction value AKs quoted. Note (2): AKs determined from method outlined in Sect.5. Note (3): Notes as follows: f = Slope alpha determined from [4.5] to [24] photometry. g = Slope alpha determined from [3.6], [5.8] and [24] photometry. Note (4): from Herbig & Dahm (2006, Cat. J/AJ/131/1530).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Jul-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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