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J/ApJ/706/762         LAEs at z∼4.5 in the LALA Cetus field        (Wang+, 2009)

Lyα-emitting galaxies at redshift z∼ 4.5 in the LALA Cetus field. Wang J.-X., Malhotra S., Rhoads J.E., Zhang H.-T., Finkelstein S.L. <Astrophys. J., 706, 762-771 (2009)> =2009ApJ...706..762W
ADC_Keywords: Galaxies, spectra ; Redshifts ; Equivalent widths ; Surveys Keywords: cosmology: observations - early universe - galaxies: evolution - galaxies: formation - galaxies: high-redshift Abstract: We present a large sample of Lyα-emitting galaxies (LAEs) spectroscopically confirmed at redshift z∼4.5, based on Inamori-Magellan Areal Camera and Spectrograph spectroscopic observations of candidate z∼4.5 Lyα-emitting galaxies in the large area Lyman alpha (LALA) narrowband imaging survey Cetus field. We identify 110 of them as z∼4.5 Lyα emitters based on single-line detections with no continuum emission blueward of the line. Six foreground galaxies are identified, either based on multiple lines or blueward continuum emission. The Lyα confirmation rate varies from <50% to 76% for candidates selected in different narrowband filters at slightly different redshifts. The sample includes many objects with equivalent widths (EWs)≳200Å. These large EW candidates are spectroscopically confirmed at the same rate as candidates with more modest EWs. Description: We obtained the narrowband images used to select z∼4.5 Lyα galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)∼80Å. The central wavelengths are 6559, 6611, 6650, 6692, and 6730Å for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in BW, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi & Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z∼4.5 Lyα emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ∼7Å. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 48 110 IMACS spectroscopically confirmed Lyα emitters at z∼4.5 in the LALA Cetus field
See also: J/ApJ/704/548 : Photometric properties of galaxies at z=4-6 (Overzier+, 2009) J/ApJ/696/546 : Lyα emitters at z∼4.86 (Shioya+, 2009) J/ApJ/671/1227 : Lyα galaxies at z∼4.5 (Dawson+, 2007) J/A+A/461/823 : Candidate Lyα emitting galaxies (Venemans+, 2007) J/ApJ/669/765 : Chandra X-ray sources in LALA Cetus field (Wang+, 2007) J/PASJ/57/881 : Imaging of high-redshift Lyman alpha emitters (Yamada+, 2005) J/AJ/127/213 : LALA Bootes field X-ray source catalog (Wang+, 2004) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 16 A16 --- [WMR2009] Target designation (JHHMMSS.s+DDMMSS) 18- 22 F5.3 --- z Spectroscopic redshift (1) 24- 28 F5.3 10-20W/m2 FLya Lyalpha line flux (2) 30- 34 F5.3 10-20W/m2 e_FLya FLya uncertainty 36 A1 --- l_EW Limit flag on EW 37- 39 I3 0.1nm EW Rest-frame equivalent width in Angstroms (3) 41- 44 I4 0.1nm E_EW ? Positive error in EW 46- 48 I3 0.1nm e_EW ? Negative error in EW
Note (1): The redshift was measured from the wavelength of the peak pixel in the line profile from one-dimensional spectra. Due to the uncertainties in the wavelength calibration (see the text for details), we expect the error in the measurement to be δz∼0.005. Note (2): The line flux was measured based on narrowband and broadband photometry, in units of 10-17erg/cm2/s. Note (3): The EW were obtained based on broadband and narrowband photometry. See Section 3.3 for details.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 14-Dec-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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