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J/MNRAS/462/2878 SFR & AGN in most luminous local universe LINERs (Povic+, 2016)

Star formation and AGN activity in the most luminous LINERs in the local universe. Povic M., Marquez I., Netzer H., Masegosa J., Nordon R., Perez E., Schoenell W. <Mon. Not. R. Astron. Soc., 462, 2878-2903 (2016)> =2016MNRAS.462.2878P (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Star Forming Region ; Morphology ; Infrared sources ; Spectroscopy Keywords: galaxies: active - galaxies: nuclei - galaxies: star formation Abstract: This work presents the properties of 42 objects in the group of the most luminous, highest star formation rate (SFR) low-ionization nuclear emission-line regions (LINERs) at z=0.04-0.11. We obtained long-slit spectroscopy of the nuclear regions for all sources, and FIR data (Herschel and IRAS) for 13 of them. We measured emission-line intensities, extinction, stellar populations, stellar masses, ages, active galactic nuclei (AGN) luminosities, and SFRs. We find considerable differences from other low-redshift LINERs, in terms of extinction, and general similarity to star-forming galaxies. We confirm the existence of such luminous LINERs in the local universe, after being previously detected at z∼0.3 by Tommasin et al. The median stellar mass of these LINERs corresponds to 6-7x1010M which was found in previous work to correspond to the peak of relative growth rate of stellar populations and therefore for the highest SFRs. Other LINERs although showing similar AGN luminosities have lower SFR. We find that most of these sources have LAGN∼LSF suggesting co-evolution of black hole and stellar mass. In general, the fraction of local LINERs on the main sequence of star-forming galaxies is related to their AGN luminosity. Description: The sources were initially selected from the SDSS/DR4 (Kauffmann et al., 2003MNRAS.341...33K; Brinchmann et al., 2004MNRAS.351.1151B) catalogue in Garching MPA-JHU based on the SDSS (http://www.sdss.org/) DR4 data (Adelman-McCarthy et al. (2006ApJS..162...38A, Cat. II/267), and references therein). LINERs were first selected using both [NII]6584/Hα and [OI]6300/Hα criteria of Kewley et al. (2006MNRAS.372..961K). Taking into account the completeness of the SDSS survey, only LINERs with 0.04<z<0.11 were selected (Netzer, 2009MNRAS.399.1907N). To eliminate LINERs ionized by pAGB stars, we selected only those galaxies with Hα EW(Hα)>2.5Å (Cid-Fernandes et al., 2011MNRAS.413.1687C). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 89 42 Summary of observations table2.dat 49 16 Summary of FIR observations with Herschel and IRAS table3.dat 19 42 Dn4000 and Hδ measurements table4.dat 56 41 The best stellar population mixture found by STARLIGHT table5.dat 112 42 Properties of strong emission lines table6.dat 119 40 Properties of extinction corrected strong emission lines table7.dat 16 40 AGN contribution measured through L(Hα) and STARLIGHT SFRs (obtained from young stellar populations) table8.dat 104 42 SFRs and AGN luminosities
See also: II/267 : The SDSS Photometric Catalog, Release 4 (Adelman-McCarthy+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 4- 5 A2 --- n_ID [*! ] Note (G1) 7- 16 F10.6 deg RAdeg Right ascension (J2000) 19- 27 F9.6 deg DEdeg Declination (J2000) 30- 34 F5.3 --- z Redshift, from SDSS public catalogues 36- 40 F5.2 mag m6500 AB continuum magnitude at 6500Å 42 A1 --- Morph Visual morphological classification (1) 44- 53 A10 "date" Date Date of observation 55- 57 F3.1 arcsec Seeing ? Average FWHM of the seeing 59- 61 I3 deg PA []? Slit position angle, orientated along the major axis 62- 63 A2 --- n_PA [PA ] PA means that the parallactic angle was used 65- 72 A8 s Texpb Total exposure time in blue parts in seconds 74- 81 A8 s Texpr Total exposure time in red parts in seconds 83- 85 F3.1 arcsec+2 Areanuc ? Area covered with our 'nuclear' extraction (2) 87- 89 A3 --- IRdata [1,2 ] Availability of Herschel (1) and IRAS (2) data
Note (1): Classification as follows: E = Elliptical/S0 S = spiral P = peculiar Note (2): just for comparison, the SDSS spectra cover an area of 7.08 arcsec2.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 5- 10 F6.4 Jy F70 ? FIR flux in the 70um Herschel/PACS band 12- 17 F6.4 Jy e_F70 ? FIR flux in the 70um Herschel/PACS band 19- 24 F6.4 Jy F160 ? FIR flux in the 160um Herschel/PACS band 26- 31 F6.4 Jy e_F160 ? FIR flux in the 160um Herschel/PACS band 33- 38 F6.4 Jy F60 ? IRAS FIR flux in 60um band 40 I1 --- q_F60 ? Quality flag on F60 (1) 42- 47 F6.4 Jy F100 ? IRAS FIR flux in 100um band 49 I1 --- q_F100 ? Quality flag on F100 (1)
Note (1): Quality flag as follows: 3 = high quality 2 = moderate quality 1 = an upper limit
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 4 A1 --- n_ID [!] Note (G1) 6- 9 F4.2 --- Dn4000 ? Strength of 4000Å break 11- 14 F4.2 --- e_Dn4000 ? rms uncertainty on Dn4000 16- 19 F4.2 --- Hd ? Balmer absorption-line index Hδ
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 4 A1 --- n_ID [!] Note (G1) 6- 10 F5.2 --- adev Goodness of the fit (see the text) 12- 16 F5.2 --- S/N Measured S/N ratio (see Section 4.2) 18- 22 F5.3 mag AV ? Extinction in V band 24- 27 F4.2 10+10Msun M* Current mass in stars 29- 33 F5.2 10+10Msun M*ini Initial mass in stars 35- 39 F5.2 % stpop1 Fraction of young stars with age[yr]≤108 41- 45 F5.2 % stpop2 Fraction of intermediate stars with 108<age[yr]≤109 47- 51 F5.2 % stpop3 Fraction of old stars with age[yr]>109 53- 56 F4.2 yr logtmean Mean age
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 4 A1 --- n_ID [!] Note (G1) 6- 9 F4.2 --- [OII] ? Flux of [OII]3272 in Hα flux unit 11- 14 F4.2 --- e_[OII] ? rms uncertainty on [OII] 16- 19 F4.2 --- Hb ? Flux of Hβ in Hα flux unit 21- 24 F4.2 --- e_Hb ? rms uncertainty on Hb 26- 29 F4.2 --- [OIII]1 ? Flux of [OIII]4959 in Hα flux unit 31- 34 F4.2 --- e_[OIII]1 ? rms uncertainty on [OIII]1 36- 39 F4.2 --- [OIII]2 Flux of [OIII]5007 in Hα flux unit 41- 44 F4.2 --- e_[OIII]2 rms uncertainty on [OIII]2 46- 49 F4.2 --- [OI] ? Flux of [OI]6300 in Hα flux unit 51- 54 F4.2 --- e_[OI] ? rms uncertainty on [OI] 56- 59 F4.2 --- [NII]1 ? Flux of [NII]6548 in Hα flux unit 61- 64 F4.2 --- e_[NII]1 ? rms uncertainty on [NII]1 66- 69 F4.2 --- [NII]2 Flux of [NII]6584 in Hα flux unit 71- 74 F4.2 --- e_[NII]2 rms uncertainty on [NII]2 76- 79 F4.2 --- [SII]1 ? Flux of [SII]6716 in Hα flux unit 81- 84 F4.2 --- e_[SII]1 ? rms uncertainty on [SII]1 86- 89 F4.2 --- [SII]2 ? Flux of [SII]6731 in Hα flux unit 91- 94 F4.2 --- e_[SII]2 ? rms uncertainty on [SII]2 96-101 F6.2 10-19mW/m2 FHa Hα flux 103-106 F4.2 10-19mW/m2 e_FHa rms uncertainty on FHA 108-112 F5.2 0.1nm EWHa Hα equivalent width (1)
Note (1): measured in the spectrum before the subtraction of the best model for the underlying stellar population.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 4 A1 --- n_ID [!] Note (G1) 6- 9 F4.2 --- [OII] ? Extinction corrected flux of [OII]3272 in Hα flux unit 11- 14 F4.2 --- e_[OII] ? rms uncertainty on [OII] 16- 19 F4.2 --- [OIII]1 ? Extinction corrected flux of [OIII]4959 in Hα flux unit 21- 24 F4.2 --- e_[OIII]1 ? rms uncertainty on [OIII]1 26- 29 F4.2 --- [OIII]2 Extinction corrected flux of [OIII]5007 in Hα flux unit 31- 34 F4.2 --- e_[OIII]2 rms uncertainty on [OIII]2 36- 39 F4.2 --- [OI] ? Extinction corrected flux of [OI]6300 in Hα flux unit 41- 44 F4.2 --- e_[OI] ? rms uncertainty on [OI] 46- 49 F4.2 --- [NII]1 ? Extinction corrected flux of [NII]6548 in Hα flux unit 51- 54 F4.2 --- e_[NII]1 ? rms uncertainty on [NII]1 56- 59 F4.2 --- [NII]2 Extinction corrected flux of [NII]6584 in Hα flux unit 61- 64 F4.2 --- e_[NII]2 rms uncertainty on [NII]2 66- 69 F4.2 --- [SII]1 ? Extinction corrected flux of [SII]6716 in Hα flux unit 71- 74 F4.2 --- e_[SII]1 ? rms uncertainty on [SII]1 76- 79 F4.2 --- [SII]2 ? Extinction corrected flux of [SII]6731 in Hα flux unit 81- 84 F4.2 --- e_[SII]2 ? rms uncertainty on [SII]2 86- 92 F7.2 10-19mW/m2 FHa Hα flux 94- 99 F6.2 10-19mW/m2 e_FHa rms uncertainty on FHA 101-106 F6.2 10+33W LHa Hα luminosity 108-112 F5.2 10+33W e_LHa rms uncertainty on LHA 114-119 F6.3 mag AV Interstellar extinction parameter in the V band
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 6- 10 F5.2 10+33W L(Ha)test Hα luminosity obtained from the STARLIGHT SFRs correspondent only to young stellar populations 12- 16 F5.1 % AGNcont Approximation of AGN contribution to Hα luminosity
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ID MLLINER identification 6- 9 F4.2 --- SFR1 SFR measured through the starlight best-fitting model using only young (age<108) stars 11- 15 F5.2 --- SFR2 SFR measured through the starlight best-fitting model using young and intermediate (age<109) stars 17- 20 F4.2 --- SFRtot Total SFR obtained from the best-fitting model 22- 25 F4.2 --- e_SFRtot rms uncertainty on SFRtot 27- 31 F5.2 --- SFRtotsc Total SFR obtained from the best-fitting model scaled to the entire galaxy 33- 36 F4.2 --- e_SFRtotsc rms uncertainty on SFRtotsc 38- 42 F5.2 --- SFRDn ? SFR measured using the Dn4000 index 44- 47 F4.2 --- e_SFRDn ? rms uncertainty on SFRDn4000 49- 53 F5.2 --- SFRDnsc ? SFR measured using the Dn4000 index scaled to the entire galaxy 55- 59 F5.2 --- e_SFRDnsc ? rms uncertainty on SFRDn4000sc 61- 65 F5.2 --- SFRPACS ? SFRs measured through Herschel/PACS data 67- 70 F4.2 --- e_SFRPACS ? rms uncertainty on SFRPACS 72- 76 F5.2 --- SFRIRAS ? SFRs measured through IRAS FIR data 78- 81 F4.2 --- e_SFRIRAS ? rms uncertainty on SFRIRAS 83- 87 F5.2 [10-7W] logLAGN ? AGN luminosity, measured through Hα and [OIII]5007 extinction corrected emission lines 89- 92 F4.2 [10-7W] e_logLAGN ? rms uncertainty on logLAGN 94- 98 F5.2 [Msun] logMtot ? Total stellar mass, measured by MPA-JHU team using SDSS DR7 data 100-103 F4.2 [Msun] logMBH ? Black hole mass measured for galaxies classified as E 104 A1 --- n_logMBH [*] * for B13 that is classified as S
Global notes: Note (G1): Notes as follows: * = sources observed with NOT ! = sources are possibly Sy2 galaxies and not LINERs as explained in Section 4.3
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 14-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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