J/ApJS/192/5 Emission-line galaxies from HETDEX pilot survey (Adams+, 2011) ================================================================================ The HETDEX pilot survey. I. Survey design, performance, and catalog of emission-line galaxies. Adams J.J., Blanc G.A., Hill G.J., Gebhardt K., Drory N., Hao L., Bender R., Byun J., Ciardullo R., Cornell M.E., Finkelstein S.L., Fry A., Gawiser E., Gronwall C., Hopp U., Jeong D., Kelz A., Kelzenberg R., Komatsu E., MacQueen P.J., Murphy J., Odoms P.S., Roth M., Schneider D.P., Tufts J.R., Wilkinson C.P. =2011ApJS..192....5A ================================================================================ ADC_Keywords: Galaxies, optical ; Equivalent widths ; Redshifts ; Surveys Keywords: cosmology: observations - galaxies: evolution - galaxies: formation - galaxies: high-redshift Abstract: We present a catalog of emission-line galaxies selected solely by their emission-line fluxes using a wide-field integral field spectrograph. This work is partially motivated as a pilot survey for the upcoming Hobby-Eberly Telescope Dark Energy Experiment. We describe the observations, reductions, detections, redshift classifications, line fluxes, and counterpart information for 397 emission-line galaxies detected over 169arcmin^2^ with a 3500-5800{AA} bandpass under 5{AA} full-width-half-maximum (FWHM) spectral resolution. The survey's best sensitivity for unresolved objects under photometric conditions is between 4 and 20x10^-17^erg/s/cm^2^ depending on the wavelength, and Ly{alpha} luminosities between 3x10^42^ and 6x10^42^erg/s are detectable. This survey method complements narrowband and color-selection techniques in the search of high-redshift galaxies with its different selection properties and large volume probed. The four survey fields within the COSMOS, GOODS-N, MUNICS, and XMM-LSS areas are rich with existing, complementary data. We find 105 galaxies via their high-redshift Ly{alpha} emission at 1.944arcmin^2^ which appear to be extended Ly{alpha} nebulae. We also find three high-z objects with rest-frame Ly{alpha} EW above the level believed to be achievable with normal star formation, EW0>240{AA}. Description: We obtained regular fall/winter/spring dark time observations from 2007 September to 2010 February on the McDonald 2.7m Harlan J. Smith telescope with the Visible Integral-field Replicable Unit Spectrograph Prototype (VIRUS-P). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 94 4 Ancillary broadband imaging properties table3.dat 98 479 HETDEX pilot survey emission line catalog table4.dat 112 479 HETDEX pilot survey emission line classifications -------------------------------------------------------------------------------- See also: J/MNRAS/401/294 : Optical identification of XMM-LSS sources (Stalin+, 2010) J/A+A/490/879 : XMM-LSS field optical identifications (Tasse+, 2008) J/ApJ/667/79 : Ly{alpha} emission-line galaxies at z=3.1 (Gronwall+, 2007) J/ApJ/653/1004 : Galaxies at 1.4<~z<~3.0 in GOODS-North Field (Reddy+, 2006) J/AJ/130/2584 : KISS emission-line galaxy candidates. IV (Salzer+, 2005) J/AJ/112/1335 : Hubble Deep Field observations (Williams+ 1996) Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 A9 --- Field Field name (1) 11- 12 I2 h RAh Central hour of right ascension (J2000) 14- 15 I2 min RAm Central minute of right ascension (J2000) 17- 18 I2 s RAs Central second of right ascension (J2000) 20 A1 --- DE- Declination sign (J2000) 21- 22 I2 deg DEd Central degree of declination (J2000) 24- 25 I2 arcmin DEm Central arcminute of declination (J2000) 27- 28 I2 arcsec DEs Central arcsecond of declination (J2000) 30- 34 F5.3 mag E(B-V) Galactic extinction value 36- 62 A27 --- Filt Filters 64 A1 --- f_Filt [a] Flag for u filter 66- 69 F4.2 arcsec Seeing The worst seeing FWHM to which all bands are matched 71- 79 A9 --- Stack Filters combined to form the detection image 81- 84 A4 --- BandK The band chosen for Kron aperture measurement 86- 89 F4.1 --- Depth The 5{sigma} limit in AB magnitudes for a point source in a 2" aperture for the band with the Kron aperture measurement 91- 94 F4.1 arcmin2 Area Visible Integral-field Replicable Unit Spectrograph Prototype (VIRUS-P) area -------------------------------------------------------------------------------- Note (1): Fields as follows: COSMOS = from the Cosmological Evolution Survey (Scoville et al. 2007ApJS..172....1S), GOODS-N = from the surrounding Great Observatories Origins Deep Survey North (Dickinson et al. 2003mglh.conf..324D), XMM-LSS = from the XMM Large-Scale Structure field (Pierre et al. 2004JCAP...09..011P) MUNICS = from the Munich Near-IR Cluster Survey (Drory et al. 2001MNRAS.325..550D). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- HPS [1/479] HETDEX Pilot Survey index number 5- 6 I2 h RAh Hour of Right Ascension (J2000) 8- 9 I2 min RAm Minute of Right Ascension (J2000) 11- 15 F5.2 s RAs Second of Right Ascension (J2000) 17 A1 --- DE- Sign of the Declination (J2000) 18- 19 I2 deg DEd Degree of Declination (J2000) 21- 22 I2 arcmin DEm Arcminute of Declination (J2000) 24- 28 F5.2 arcsec DEs Arcsecond of Declination (J2000) 30- 36 F7.2 0.1nm lambda Observed emission wavelength (1) 38- 41 I4 km/s FWHM Emission line intrinsic FWHM (2) 43- 47 F5.1 --- S/N Emission line Signal-to-Noise 49- 54 F6.1 10-20W/m2 Flux Emission line flux (in 10^-17^erg/cm^2^/s) (3) 56- 59 F4.1 10-20W/m2 e_Flux Lower limit uncertainty in Flux 61- 64 F4.1 10-20W/m2 E_Flux Upper limit uncertainty in Flux 66- 69 F4.1 arcsec Spat Emission line spatial FWHM (3) 71- 73 F3.1 arcsec e_Spat Lower limit uncertainty in Spatial 75- 77 F3.1 arcsec E_Spat Upper limit uncertainty in Spatial 79- 98 A20 --- Match Indices that share position and redshift -------------------------------------------------------------------------------- Note (1): In a vacuum, heliocentric frame (Angstroms) with an estimated 0.5{AA} uncertainty based on simulations. Note (2): After removal of a 5 Angstrom FWHM instrumental resolution and with an estimated 300km/s uncertainty. Note (3): As measured with the curve of growth method. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- HPS [1/479] HETDEX Pilot Survey index number 5- 19 A15 --- xid Best continuum-selected counterpart (JHHMMSSs+DDMMSS) 21- 25 F5.2 mag mag ? Counterpart R or i' band magnitude (1) 27- 30 F4.2 --- Prob Probability of counterpart association 32- 37 F6.1 0.1nm EW Rest-frame equivalent width (2) 39- 43 F5.1 0.1nm e_EW Lower limit uncertainty in EW 45- 50 F6.1 0.1nm E_EW Upper limit uncertainty in EW 52- 57 F6.1 0.1nm EWint Interpolated rest-frame equivalent width (3) 59- 64 F6.1 0.1nm e_EWint Lower limit uncertainty in EWint 66- 71 F6.1 0.1nm E_EWint Upper limit uncertainty in EWint 73- 83 A11 --- Trans Emission line transition (4) 85- 90 F6.4 --- z Estimated redshift 92- 95 F4.2 --- Lya Probability emission line is Ly{alpha} (5) 97-112 A16 --- X-ray X-ray counterpart identification (JHHMMSSs+DDMMSS) -------------------------------------------------------------------------------- Note (1): See table 2 for the Johnson or SDSS R-band filters used. The MUNICS field, at {alpha}~3hr, instead uses an SDSS i filter. Note (2): For this counterpart and the selected transition based on the R-band photometry, or the i'-band in MUNICS where no R-band is available. Note (3): For this counterpart and the selected transition based on an interpolation between the two nearest filters. Note (4): Based on the EW cut and/or the presence of multiple emission lines. Note (5): As calculated by marginalizing over all potential counterpart. -------------------------------------------------------------------------------- History: From electronic version of the journal References: Blanc et al. Paper II. 2011ApJ...736...31B Cat. J/ApJ/736/31 Finkelstein et al. Paper III. 2011ApJ...729..140F ================================================================================ (End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 22-Mar-2011