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J/ApJ/819/73       Metallicity evolution of COSMOS BCD sample      (Lian+, 2016)

The metallicity evolution of blue compact dwarf galaxies from the intermediate redshift to the local universe. Lian J., Hu N., Fang G., Ye C., Kong X. <Astrophys. J., 819, 73 (2016)> =2016ApJ...819...73L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Equivalent widths ; Redshifts ; Extinction ; Abundances Keywords: galaxies: dwarf - galaxies: evolution - galaxies: fundamental parameters - galaxies: star formation Abstract: We present oxygen abundance measurements for 74 blue compact dwarf (BCD) galaxies in the redshift range of [0.2, 0.5] using the strong-line method. The spectra of these objects are taken using Hectospec on the Multiple Mirror Telescope. More than half of these BCDs had dust attenuation corrected using the Balmer decrement method. For comparison, we also selected a sample of 2023 local BCDs from the Sloan Digital Sky Survey (SDSS) database. Based on the local and intermediate-z BCD samples, we investigated the cosmic evolution of the metallicity, star formation rate (SFR), and Dn(4000) index. Compared with local BCDs, the intermediate-z BCDs had a systematically higher R23 ratio but a similar O32 ratio. Interestingly, no significant deviation in the mass-metallicity (MZ) relation was found between the intermediate-z and local BCDs. Besides the metallicity, the intermediate-z BCDs also exhibited an SFR distribution that was consistent with local BCDs, suggesting a weak dependence on redshift. The intermediate-z BCDs seemed to be younger than the local BCDs with lower Dn(4000) index values. The insignificant deviation in the mass-metallicity and mass-SFR relations between intermediate-z and local BCDs indicates that the relations between the global parameters of low-mass compact galaxies may be universal. These results from low-mass compact galaxies could be used to place important observational constraints on galaxy formation and evolution models. Description: To study low-mass galaxies outside the local universe, we selected a blue compact dwarf (BCD) sample at intermediate redshift in the Cosmic Evolution Survey (COSMOS) deep field and then performed followup spectroscopic observation using Hectospec on the Multiple Mirror Telescope (MMT). We selected the BCD sample from a public Ks selected catalog of the COSMOS field (Muzzin et al. 2013, J/ApJS/206/8). The observations of these BCDs using the Hectospec/MMT were carried out in 2015 February. Each fiber has a diameter of 1.5" (corresponding to 5 kpc at z=0.2) and covers most of the light of BCDs at intermediate redshift. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 85 74 Emission Line Measurements of COSMOS BCD Sample table2.dat 42 74 Physical Properties of COSMOS BCD Sample
See also: J/ApJS/147/29 : BRHalpha data of blue compact dwarf galaxies (Gil De Paz+, 2003) J/A+A/429/115 : JHK' photometry of Blue Compact Dwarf Galaxies (Noeske+, 2005) J/A+A/434/887 : HI data of blue compact dwarf galaxies (Huchtmeier+, 2005) J/ApJS/156/345 : Surface photometry of BCD galaxies (Gil de Paz+, 2005) J/ApJS/206/8 : COSMOS/UltraVISTA Ks-selected catalogs v4.1 (Muzzin+, 2013) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 I2 --- ID [1/74] Source identification number 4- 5 I2 h RAh Hour of Right Ascension (J2000) 7- 8 I2 min RAm Minute of Right Ascension (J2000) 10- 14 F5.2 s RAs Second of Right Ascension (J2000) 16 A1 --- DE- Sign of the Declination (J2000) 17- 18 I2 deg DEd Degree of Declination (J2000) 20- 21 I2 arcmin DEm Arcminute of Declination (J2000) 23- 26 F4.1 arcsec DEs Arcsecond of Declination (J2000) 28- 33 F6.1 10-21W/m2 F3727 Flux of [OII]λ3727 line (in 10-18erg/s/cm2) 35- 37 F3.1 10-21W/m2 e_F3727 Uncertainty in F3727 39- 43 F5.1 10-21W/m2 FHg ? Hγ line flux 45- 47 F3.1 10-21W/m2 e_FHg ? Uncertainty in FHg 49- 53 F5.1 10-21W/m2 FHb Hβ line flux 55- 57 F3.1 10-21W/m2 e_FHb Uncertainty in FHb 59- 63 F5.1 0.1nm EW(Hb) Equivalent width of Hβ (Å) 65- 70 F6.1 10-21W/m2 F4959 Flux of [OIII]λ4959 line (in 10-18erg/s/cm2) 72- 74 F3.1 10-21W/m2 e_F4959 Uncertainty in F4959 76- 81 F6.1 10-21W/m2 F5007 Flux of [OIII]λ5007 line (in 10-18erg/s/cm2) 83- 85 F3.1 10-21W/m2 e_F5007 Uncertainty in F5007
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 I2 --- ID [1/74] Source identification number 4- 8 F5.3 --- z Redshift 10- 12 F3.1 mag Av Dust extinction 13 A1 --- n_Av [s] Note on Av (1) 15- 18 F4.2 [Msun] logM* Log of stellar mass 20- 23 F4.2 --- 12+log(O/H) Oxygen abundance 25- 28 F4.2 --- e_12+log(O/H) Uncertainty in 12+log(O/H) 30- 33 F4.2 [Msun/yr] log(SFR) Log of star formation rate (2) 35- 38 F4.2 [Msun/yr] e_log(SFR) Uncertainty in log(SFR) 40- 42 F3.1 --- Dn(4000) ? Dn(4000) index (3)
Note (1): Note as follows: s = Dust attenuation AV from SED fitting. Note (2): The listed SFR are not corrected for burst age which can be done by combining the EW(Hb) listed in Table 1 and Equation (5) in Izotov et al. (2015MNRAS.451.2251I). Note (3): We calculated the 4000 Å break [i.e., Dn(4000) index] based on the definition of Balogh et al. (1999ApJ...527...54B).
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 01-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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