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J/AJ/154/113       Magellan/M2FS spectroscopy of Abell 267       (Tucker+, 2017)

Magellan/M2FS spectroscopy of galaxy clusters: stellar population model and application to Abell 267. Tucker E., Walker M.G., Mateo M., Olszewski E.W., Bailey J.I., Crane J.D., Shectman S.A. <Astron. J., 154, 113-113 (2017)> =2017AJ....154..113T (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, spectra ; Abundances, [Fe/H] ; Abundances ; Velocity dispersion Keywords: galaxies: clusters: individual: Abell 267 - galaxies: general - techniques: imaging spectroscopy Abstract: We report the results of a pilot program to use the Magellan/M2FS spectrograph to survey the galactic populations and internal kinematics of galaxy clusters. For this initial study, we present spectroscopic measurements for 223 quiescent galaxies observed along the line of sight of the galaxy cluster Abell 267 (z∼0.23). We develop a Bayesian method for modeling the integrated light from each galaxy as a simple stellar population, with free parameters that specify the redshift (vlos/c) and characteristic age, metallicity ([Fe/H]), alpha-abundance ([α/Fe]), and internal velocity dispersion (σint) for individual galaxies. Parameter estimates derived from our 1.5hr observation of A267 have median random errors of σVlos=20km/s, σAge=1.2Gyr, σ[Fe/H]=0.11dex, σ[α/Fe]=0.07dex, and σσint=20km/s. In a companion paper, we use these results to model the structure and internal kinematics of A267. Description: We select targets for Michigan/Magellan Fiber System (M2FS) observations by identifying galaxies detected in SDSS images (Data Release 12; Alam et al.2015, Cat. V/147) that are projected along the line of sight to Abell 267 and are likely to be quiescent cluster members. We observed 223 individual galaxy spectra on 2013 November 30 on the Clay Magellan Telescope using M2FS. We used the low-resolution grating on M2FS and chose a coverage range of 4600-6400Å with a resolution of R∼2000. The detector used with M2FS consists of two 4096*4112 pixel CCDs. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 100 223 Results for fitting of A267 spectra
See also: V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015) J/ApJ/819/53 : Magellan/M2FS spectroscopy of Tucana 2 & Grus 1 (Walker+, 2016) J/ApJ/797/106 : Redshifts in nine galaxy cluster fields (Hwang+, 2014) J/ApJ/767/15 : Hectospec Cluster Survey (HeCS) (Rines+, 2013) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/223] Michigan/Magellan Fiber System (M2FS) target, sequential identifier 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- 27 F4.1 arcsec DEs Arcsecond of Declination (J2000) 29- 33 F5.2 mag rmag [18.8/21.1] SDSS r band magnitude 35- 39 F5.2 mag imag [18.4/20.7] SDSS i band magnitude 41- 44 F4.1 --- S/N [0.6/32.2] Median spectral Signal-to-Noise per pixel 46- 51 I6 km/s <Vlos> [11012/133103] Mean Line-of-Sight velocity, solar rest frame (Vlos) 53- 57 I5 km/s e_<Vlos> [7/45300] Uncertainty in <Vlos> 59- 62 F4.1 Gyr <Age> [0.4/14.8] Mean inferred age 64- 66 F3.1 Gyr e_<Age> [0.2/5.2] Uncertainty in <Age> 68- 72 F5.2 [Sun] <Fe/H> [-3.4/0.5] Mean metallicity relative to Sun 74- 77 F4.2 [Sun] e_<Fe/H> [0.03/0.8] Uncertainty in <Fe/H> 79- 83 F5.2 --- <a/Fe> [-0.1/0.8] Mean chemical abundance [α/Fe] 85- 88 F4.2 --- e_<a/Fe> [0.01/0.4] Uncertainty in <a/Fe> 90- 94 F5.1 km/s <sigma> [28/437.6] Mean internal velocity dispersion σint 96-100 F5.1 km/s e_<sigma> [3.1/121.2] Uncertainty in <sigma>
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 07-Feb-2018
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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