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J/ApJ/697/1410          Lyman break galaxies at z∼1.8-2.8            (Ly+, 2009)

Lyman break galaxies at z ∼ 1.8-2.8: GALEX/NUV imaging of the Subaru Deep Field. Ly C., Malkan M.A., Treu T., Woo J.-H., Currie T., Hayashi M., Kashikawa N., Motohara K., Shimasaku K., Yoshida M. <Astrophys. J., 697, 1410-1432 (2009)> =2009ApJ...697.1410L
ADC_Keywords: Galaxies, photometry ; Redshifts ; Spectroscopy Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: luminosity function, mass function - galaxies: photometry Abstract: A photometric sample of ∼8000 V<25.3 candidate Lyman break galaxies (LBGs) has been selected by combining Subaru/Suprime-Cam BVRCi'z' optical data with deep GALEX/NUV imaging of the Subaru Deep Field. Follow-up spectroscopy confirmed 24 LBGs at 1.5≲z≲2.7. Among the optical spectra, 12 have Lyα emission with rest-frame equivalent widths of ∼5-60Å. The success rate for identifying LBGs as NUV-dropouts at 1.5<z<2.7 is 86%. The rest-frame UV (1700Å) luminosity function (LF) is constructed from the photometric sample with corrections for stellar contamination and z<1.5 interlopers (lower limits). The LF is 1.7±0.1 (1.4±0.1 with a hard upper limit on stellar contamination) times higher than those of z∼2 BXs and z∼3 LBGs. Description: The Subaru Deep Field (SDF; Kashikawa et al. 2004PASJ...56.1011K), centered at RA=13h24m38.9s, DE=+27°29'25.9", is a deep wide-field (857.5arcmin2) extragalactic survey with optical data obtained from Suprime-Cam mounted on the Subaru Telescope. It was imaged with GALEX in the NUV(1750-2750Å) between 2005 March 10 and 2007 May 29 (GI1-065) with a total integration time of 138176s. The Keck Low-Resolution Imaging and Spectrograph (LRIS) was used to target candidate LBGs in multislit mode on 2007 January 23-25. Spectra of NUV-dropouts from the final photometric catalog were obtained with the multifiber optical spectrograph Hectospec on the 6.5m MMT on 2008 March 13 and April 10, 11, and 14. Spectra of BzKs were obtained on 2007 May 3-4 with Subaru using the Multi-Object Infrared Camera and Spectrograph (MOIRCS). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 130 75 Properties of spectroscopically targeted NUV-dropouts and BzKs
See also: B/subaru : Log of Subaru Prime Focus Camera Exposures (ADAC NAOJ, 2007) J/MNRAS/401/1521 : Stellar masses of Lyman break galaxies at z∼3 (Magdis+, 2010) J/MNRAS/380/986 : Lyman-break galaxies from GALEX (Burgarella+, 2007) J/ApJ/657/738 : SDF galaxies multi-photometry (Ly+, 2007) J/PASJ/58/313 : Lyα emitters in the SUBARU Deep Field (Shimasaku+, 2006) J/PASJ/57/165 : Lyα emitters in the SUBARU Deep Field (Taniguchi+, 2005) J/ApJ/592/728 : Lyman break galaxies at redshift z∼3 (Steidel+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Sample Sample (1) 7- 13 A7 --- B-ID B-band catalog from SExtractor identification (2) 15- 32 A18 --- Name SDF name (HHMMSS.s+DDMMSS.ss; J2000) 34 A1 --- l_NUV-B Limit flag on NUV-B 35- 39 F5.3 mag NUV-B NUV-B band color index 41- 46 F6.3 mag B-V B-V color index 48 A1 --- l_NUV Limit flag on NUV 49- 54 F6.3 mag NUV GALEX NUV AB magnitude 56- 61 F6.3 mag Bmag Subaru B-band AB magnitude 63- 68 F6.3 mag Vmag Subaru V-band AB magnitude 70- 75 F6.3 mag Rcmag Subaru Rc band AB magnitude 77- 82 F6.3 mag i'mag Subaru i'-band AB magnitude 84- 89 F6.3 mag z'mag Subaru z'-band AB magnitude 91- 97 F7.4 --- z ? Cross-correlated redshift 99 A1 --- f_z [d] low S/N (3) 101-105 F5.2 --- R ? Cross-correlation signal to noise 107-116 A10 --- Temp Template yielding the highest R value (4) 118-122 F5.1 zW/m2 F(Lya) ? Lyα line flux (in units of 10-18erg/s/cm2 = 10-21W/m2) 123 A1 --- f_F(Lya) [c] Flag on F(Lya) (5) 125-129 F5.2 0.1nm EW0 ? Lyα equivalent width 130 A1 --- f_EW0 [c] u,nusual Lyalpha profile (5)
Note (1): Sample as follows: ELS = With emission lines ALS = Absorption line systems Z>1.5 = z>1.5 interlopers and stars Amb = Ambiguous NUV-dropouts Und = Undetected NUV-dropouts Note (2): Identified sources are based on an R>3.0 criterion (exceptions are AGNs, stars, and those with emission lines). The character following the ID number corresponds to the spectrograph used: "H" = Hectospec, "L" = LRIS, "M" = MOIRCS. Note (3): d = The values reported here correspond to the best cross-correlated results, but may be wrong due to the low S/N of the spectra. Note (4): * the values 1 to 4 correspond to the four spectra of Steidel et al. (2003, Cat. J/ApJ/592/728) from strongest Lyα absorption to emission; * the values 5 and 6 refer to the Shapley et al. (2003ApJ...588...65S) composite and cB58 spectra (spectra of MS 1512-cB58 from Pettini et al. 2000ApJ...528...96P), respectively. * the value 7 corresponds to the rest-frame NUV spectra from Savaglio et al. (2004ApJ...602...51S), and "AGN" refers to a SDSS QSO template. * For interlopers, the six SDSS composite spectra presented in Yip et al. (2004AJ....128..585Y) correspond to [1] to [6] from strongest absorption-line to strongest emission-line systems. [7], [8], and [9] correspond to the rvsao templates "femtemp," "EA," and "eatemp," respectively. Note (5): c = As discussed in the Appendix, this source shows an unusual Lyα profile, so the reported flux and rest-frame EW excluded the blue excess by deblending in IRAF splot.
Nomenclature Notes: Table 1: galaxies are <[LMT2009] SDF JHHMMSS.s+DDMMSS.ss> in Simbad. History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-May-2011
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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