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J/AJ/141/14         HST WFC3 ERS : emission-line galaxies    (Straughn+, 2011)

Hubble Space Telescope WFC3 Early Release Science: emission-line galaxies from infrared grism observations. Straughn A.N., Kuntschner H., Kummel M., Walsh J.R., Cohen S.H., Gardner J.P., Windhorst R.A., O'Connell R.W., Pirzkal N., Meurer G., McCarthy P.J., Hathi N.P., Malhotra S., Rhoads J., Balick B., Bond H.E., Calzetti D., Disney M.J., Dopita M.A., Frogel J.A., Hall D.N.B., Holtzman J.A., Kimble R.A., Mutchler M., Paresce F., Saha A., Silk J.I., Trauger J.T., Walker A.R., Whitmore B.C., Young E.T., Xu C. <Astron. J., 141, 14 (2011)> =2011AJ....141...14S
ADC_Keywords: Galaxies, IR ; Redshifts ; Spectroscopy ; Equivalent widths Keywords: catalogs - galaxies: starburst - techniques: spectroscopic Abstract: We present grism spectra of emission-line galaxies (ELGs) from 0.6 to 1.6um from the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope. These new infrared grism data augment previous optical Advanced Camera for Surveys G800L 0.6-0.95um grism data in GOODS-South from the PEARS program, extending the wavelength coverage well past the G800L red cutoff. The Early Release Science (ERS) grism field was observed at a depth of two orbits per grism, yielding spectra of hundreds of faint objects, a subset of which is presented here. ELGs are studied via the Hα, [OIII], and [OII] emission lines detected in the redshift ranges 0.2~<z~<1.4, 1.2~<z~<2.2, and 2.0~<z~<3.3, respectively, in the G102 (0.8-1.1um; R~=210) and G141 (1.1-1.6um; R~=130) grisms. Description: The ERS II program for WFC3 consists of both UV and IR observations of about 30% of the GOODS-South field (Giavalisco et al., 2004, Cat. II/261). Here we summarize the ERS II program; Windhorst et al. (2011ApJS..193...27W) present the ERS II data reduction effort in detail. Eight pointings were imaged with the UVIS channel (UV filters F225W, F275W, and F336W at depths of 2 orbits/pointing/filter for F225W and F275W and 1 orbit/pointing for F336W) and ten with the IR channel (filters F098M, F125W, F160W) at 2 orbits/pointing/filter. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 86 73 Global properties of 51 emission-line galaxies (ELG)
See also: II/261 : GOODS initial results (Giavalisco+, 2004) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID [3/583] ID number <[SKK2011] NNN> in Simbad 4 A1 --- n_ID [ab] Note on source (1) 6- 15 F10.7 deg RAdeg Right ascension in decimal degrees (J2000) 17- 27 F11.7 deg DEdeg Declination in decimal degrees (J2000) 29- 33 F5.2 mag F098M HST/WFC3 F098M (Ys) AB magnitude 35- 39 I5 0.1nm lambda [800/16636] Wavelength of line 41- 46 F6.1 zW/m2 Flux ?=- Flux (10-18erg/cm2/s) (2) 48- 50 I3 zW/m2 e_Flux ? rms uncertainty on Flux 52- 54 I3 0.1nm EW ?=- Equivalent width of line (2) 56- 72 A17 --- Line Line identification (3) 73- 76 F4.1 Msun/yr SFR ?=- Stellar formation rate (2) 78 I1 Msun/yr e_SFR ? rms uncertainty on SFR 80- 84 F5.3 --- z ?=- Grism redshift, recalculated redshift based on the line identification 86 I1 --- Flag ? Flag for source of input redshift used for line identification (4)
Note (1): Notes as follows: a = CDF-S X-ray sources identified as an AGN by Szokoly et al. (2004, Cat. J/ApJS/155/271) b = New spectroscopic redshift (no previous photometric or spectroscopic redshift measurements) Note (2): No data in the case of fluxes (and EW, SFR) indicate that the spectrum had a high level of contamination, but wavelengths were secure enough to warrant redshift determination. Note (3): No data indicates that no suitable line ID was found for the given input redshift. Note (4): Flags as follows: 1 = two lines visible in the spectrum, no prior redshift needed 2 = single line in the spectrum, line ID and grism redshift based on prior spectroscopic redshift 3 = single line in the spectrum, line ID and grism redshift based on prior photometric redshift.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 21-Jul-2012
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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