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J/ApJ/706/1364  SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)

The SINS survey: SINFONI integral field spectroscopy of z ∼ 2 star-forming galaxies. Forster Schreiber N.M., Genzel R., Bouche N., Cresci G., Davies R., Buschkamp P., Shapiro K., Tacconi L.J., Hicks E.K.S., Genel S., Shapley A.E., Erb D.K., Steidel C.C., Lutz D., Eisenhauer F., Gillessen S., Sternberg A., Renzini A., Cimatti A., Daddi E., Kurk J., Lilly S., Kong X., Lehnert M.D., Nesvadba N., Verma A., McCracken H., Arimoto N., Mignoli M., Onodera M. <Astrophys. J., 706, 1364-1428 (2009)> =2009ApJ...706.1364F
ADC_Keywords: Galaxies, spectra ; Surveys ; Spectroscopy ; Redshifts ; Equivalent widths ; Photometry Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: kinematics and dynamics - infrared: galaxies Abstract: We present the Spectroscopic Imaging survey in the near-infrared (near-IR) with SINFONI (SINS) of high-redshift galaxies. With 80 objects observed and 63 detected in at least one rest-frame optical nebular emission line, mainly Hα, SINS represents the largest survey of spatially resolved gas kinematics, morphologies, and physical properties of star-forming galaxies at z∼1-3. We describe the selection of the targets, the observations, and the data reduction. We then focus on the "SINS Hα sample," consisting of 62 rest-UV/optically selected sources at 1.3<z<2.6 for which we targeted primarily the Hα and [NII] emission lines. Only ∼30% of this sample had previous near-IR spectroscopic observations. The galaxies were drawn from various imaging surveys with different photometric criteria; as a whole, the SINS Hα sample covers a reasonable representation of massive M*≳1010M star-forming galaxies at z∼1.5-2.5, with some bias toward bluer systems compared to pure K-selected samples due to the requirement of secure optical redshift. The Hα morphologies tend to be irregular and/or clumpy. About one-third of the SINS Hα sample galaxies are rotation-dominated yet turbulent disks, another one-third comprises compact and velocity dispersion-dominated objects, and the remaining galaxies are clear interacting/merging systems; the fraction of rotation-dominated systems increases among the more massive part of the sample. Description: The observations of the SINS Hα sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R∼1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R∼2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 116 80 SINS survey: galaxies observed table2.dat 125 62 Photometric properties of the SINS Hα sample galaxies table3.dat 116 62 Properties derived from SED modeling of the SINS Hα sample galaxies table6.dat 75 62 Hα properties of the SINS Hα sample table7.dat 140 62 Hα luminosities and equivalent widths of the SINS Hα sample table8.dat 122 62 Star formation rate estimates of the SINS Hα sample table9.dat 137 47 Dynamical properties and mass estimates of the SINS Hα sample refs.dat 103 37 References
See also: II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007) VII/228 : Las Campanas Infrared Survey (Chen+, 2001-2002) J/ApJ/682/985 : FIREWORKS photometry of GOODS CDF-S (Wuyts+, 2008) J/ApJS/172/70 : zCOSMOS-bright catalog (Lilly+, 2007) J/A+A/462/553 : EIS: optical deep public survey (Mignano+, 2007) J/ApJ/647/128 : Hα observations of UV-selected galaxies (Erb, 2006) J/A+A/437/883 : K20 survey: spectroscopic catalogue (Mignoli+, 2005) J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005) J/AJ/127/2455 : Gemini Deep Deep Survey (GDDS) (Abraham+, 2004) J/ApJ/616/71 : Optical properties of SCUBA galaxies (Smail+, 2004) J/ApJ/592/728 : Lyman break galaxies at redshift z∼3 (Steidel+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 23 A23 --- Name Galaxy name 24- 26 A3 --- f_Name [cehjl, ] Flag(s) on target galaxy (1) 28- 33 F6.4 --- zsp Spectroscopic redshift (2) 34 A1 --- n_zsp [gik] Note on redshift (3) 36- 56 A21 --- Class Selection class (4) 58 A1 --- l_Kmag Limit flag on Kmag 59- 63 F5.2 mag Kmag ? K-band magnitude (Vega system) 64 A1 --- n_Kmag [dfim] Note on Kmag (3) 66- 93 A28 --- Survey Parent survey or field 95-116 A22 --- Ref Reference(s) (see refs.dat file)
Note (1): Flag as follows: c = These galaxies are known to host an AGN based on their optical (rest-UV) spectrum, or near-IR (rest-optical) spectrum from either previous long-slit observations or our SINFONI data. For all of those detected with SINFONI, clear signs of AGN activity are identified (from the [NII]/Hα line ratio and/or the line widths). For K20-ID5, the rest-frame optical emission characteristics were argued by van Dokkum et al. (2005ApJ...622L..13V) to be more consistent with starburst-driven shock excitation rather than AGN activity. e = Q2346-BX404 and BX405 are an interacting pair, with angular separation of 3.63", corresponding to a projected distance of 30.3kpc at the redshift of the sources. h = The SINFONI observations of GMASS-2113 targeted the catalog position reported by J. D. Kurk et al. (2009Msngr.135...40K), but a second component to the east was serendipitously detected with Hα at the same redshift; the GMASS-2113W and 2113E pair has an angular separation of 1.9", corresponding to a projected distance of 16.0kpc at the redshift of the pair. j = The SINFONI observations of SA12-8768 targeted the catalog position reported by Abraham et al. (2004, Cat. J/AJ/127/2455). A second component 2.40" to the northwest was serendipitously detected with Hα at the same redshift and at a (projected) distance of 19.8kpc. l = Radio galaxy, identified as Hα emitter by Kurk et al. (2004A&A...428..793K). Note (2): Spectroscopic redshift based on rest-frame UV emission or absorption lines (e.g., Lyα, interstellar absorption lines) obtained with optical spectroscopy, or based on Hα from near-IR long-slit spectroscopy. Note (3): Flag as follows: d = No K-band photometry was published by Erb et al. (2006ApJ...646..107E); we measured the K-band magnitude from publicly available archival imaging obtained with the SOFI instrument at the ESO NTT as part of program ID 071.A-0639 (PI: M. D. Lehnert). f = For BX 482, no K-band photometry is available. The H160-band magnitude is given, measured from deep HST/NICMOS imaging with the NIC2 camera through the F160W filter (λ∼1.6um; N. M. Forster Schreiber et al. 2009, in preparation). g = Daddi et al. (2004ApJ...600L.127D) reported an optical redshift of 2.25 but noted that is was uncertain. Our SINFONI data clearly detected the Hα and [NII] emission lines, at a redshift of 2.0343. i = GMASS-2113E is not included in the GMASS catalog but we cross-identified it in the Ks-selected FIREWORKS CDFS catalog of Wuyts et al. (2008, Cat. J/ApJ/682/985); the redshift listed is from our SINFONI Hα detection, and the photometry is taken from Wuyts et al. (2008, cat. J/ApJ/682/985). k = The Hα redshift from our SINFONI data is given. m = For these objects, the H-band magnitude is given; no K-band photometry is available. Note (4): The class corresponds to the primary selection applied in the surveys from which our SINS targets were drawn. As explained in Section 2, a number of sources satisfy more than one criteria, e.g., the majority of the K-selected objects also satisfy the sBzK color criteria. Class as follows: BX = optically selected galaxy with z∼2-2.5 BM = optically selected galaxy with z∼1.5-2 LBG = Lyman-break galaxy SMG = submillimeter selected galaxy
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Galaxy name 13 A1 --- f_Name [a] Flag on name (1) 15- 19 A5 --- Ref Photometric reference(s) (see refs.dat file) 21 A1 --- l_Bmag Limit flag on Bmag 22- 26 F5.2 mag Bmag ? B-band AB magnitude 28- 31 F4.2 mag e_Bmag ? Bmag uncertainty 33- 37 F5.2 mag Gmag ? G-band AB magnitude 39- 42 F4.2 mag e_Gmag ? Gmag uncertainty 44 A1 --- l_Hmag Limit flag on Hmag 45- 49 F5.2 mag Hmag ? H-band magnitude (Vega system) 51- 54 F4.2 mag e_Hmag ? Hmag uncertainty 56- 60 F5.2 mag Ksmag ? Ks-band magnitude 62- 65 F4.2 mag e_Ksmag ? Ksmag uncertainty 67 A1 --- l_B-Ks Limit flag on B-K 68- 71 F4.2 mag B-Ks ? Bmag-Ksmag color index 73- 76 F4.2 mag e_B-Ks ? B-Ks uncertainty 78- 81 F4.2 mag G-Ks ? Gmag-Ksmag color index 83- 86 F4.2 mag e_G-Ks ? G-Ks uncertainty 88 A1 --- l_B-z Limit flag on B-z 89- 93 F5.2 mag B-z ? Bmag-zAB color index 95- 98 F4.2 mag e_B-z ? B-z uncertainty 100 A1 --- l_z-Ks Limit flag on z-Ks 101-104 F4.2 mag z-Ks ? zAB-Ksmag color index 106-109 F4.2 mag e_z-Ks ? z-Ks uncertainty 111-114 F4.2 mag J-Ks ? JVega-Ksmag color index 116-119 F4.2 mag e_J-Ks ? J-Ks uncertainty 121-125 F5.3 mag E(B-V) E(B-V) value (2)
Note (1): a = K-band photometry is not available from Erb et al. (2006ApJ...646..107E) in the SSA22a field; we used publicly available archival Ks imaging from SOFI at the ESO NTT, obtained under program 071.A-0639 (PI: M.D. Lehnert). Note (2): All photometry has been corrected for Galactic extinction based on the dust maps and extinction curve of Schlegel et al. (1998ApJ...500..525S).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Galaxy name 14- 19 A6 --- SFH Best-fitting star formation history (3) 21- 24 I4 Myr Age ? Age 26- 29 I4 Myr E_Age ? Positive error in Age (4) 31- 34 I4 Myr e_Age ? Negative error in Age (4) 36- 38 F3.1 mag Av ? Extinction 40- 42 F3.1 mag E_Av ? Positive error in Av (4) 44- 46 F3.1 mag e_Av ? Negative error in Av (4) 48- 52 F5.2 10+10Msun Mass ? Stellar mass 54- 57 F4.2 10+10Msun E_Mass ? Positive error in Mass (4) 59- 62 F4.2 10+10Msun e_Mass ? Negative error in Mass (4) 64- 69 F6.2 mag VMag ? Rest-frame absolute V-band AB magnitude, uncorrected for extinction 71- 74 F4.2 mag E_VMag ? Positive error in VMag (4) 76- 79 F4.2 mag e_VMag ? Negative error in VMag (4) 81- 86 F6.2 Msun/yr SFR ? Star formation rate 88- 92 F5.1 Msun/yr E_SFR ? Positive error in SFR (4) 94- 99 F6.2 Msun/yr e_SFR ? Negative error in SFR (4) 101-105 F5.2 Gyr-1 sSFR ? Specific SFR (i.e., the ratio of star formation rate over stellar mass) 107-110 F4.1 Gyr-1 E_sSFR ? Positive error in sSFR (4) 112-116 F5.2 Gyr-1 e_sSFR ? Negative error in sSFR (4)
Note (3): The best-fitting star formation history as follows: CSF = constant star formation rate; tau300 = exponentially declining star formation rate with e-folding timescale of τ=300Myr. Note (4): The formal (random) fitting uncertainties are given, derived from the 68% confidence intervals based on 200 Monte Carlo simulations for the default set of Bruzual & Charlot (2003MNRAS.344.1000B) models with solar metallicity, the Chabrier (2003PASP..115..763C) IMF, and the Calzetti et al. (2000ApJ...533..682C) reddening law; systematic uncertainties (from SED modeling assumptions) are estimated to be typically ±30% for the stellar masses, ±0.3mag for the extinctions, and factors of ∼2-3 for the ages as well as for the absolute and specific star formation rates (see Section 3 and Appendix A).
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Galaxy name 14- 17 F4.2 arcsec Rap ? Radius of the circular aperture (5) 19- 24 F6.4 --- zHa Redshift (6) 25 A1 --- f_zHa [)] ): vacuum (6) 27 A1 --- l_FHa Limit flag on FHa 28- 31 F4.1 10-20W/m2 FHa Halpha flux in 10^-17^erg/s/cm^2^ (6) 33- 35 F3.1 10-20W/m2 E_FHa ? Positive error on FHa 37- 39 F3.1 10-20W/m2 e_FHa ? Negative error on FHa 41- 43 I3 km/s Sig ? Velocity dispersion (6) 45- 48 I4 km/s E_Sig ? Positive error on Sig 50- 51 I2 km/s e_Sig ? Negative error on Sig 53 A1 --- l_r1/2 Limit flag on r1/2 54- 56 F3.1 kpc r1/2 ? Intrinsic Halpha half-light radius (7) 58- 60 F3.1 kpc e_r1/2 ? r1/2 uncertainty 62- 65 F4.1 kpc FWHM ? Intrinsic FWHM size along the major axis (8) 67- 69 F3.1 kpc e_FWHM ? FWHM uncertainty 71 A1 --- l_FBB Limit flag on FBB 72- 75 F4.2 --- FBB ? Fractional contribution of the Halpha emission line to the broadband flux density (9)
Note (5): Used to extract the spatially integrated spectrum of each source. Note (6): Redshift (vacuum), flux, and velocity dispersion of Hα derived by fitting a Gaussian profile to the line emission in the spatially integrated spectrum. The velocity dispersion is corrected for spectral instrumental resolution. The uncertainties correspond to the formal 68% confidence intervals derived from 100 Monte Carlo simulations. For undetected sources, the optical redshift is given (parenthesis flag) and the 3σ upper limit on the flux is given. The limits are computed based on the noise spectrum within an aperture of radius 1", assuming Hα at the wavelength expected for the optical redshift and an intrinsic width corresponding σint=130km/s, the average for the detected sources. Note (7): Intrinsic (corrected for spatial resolution) Hα half-light radius derived from curve-of-growth analysis from spectra integrated in circular apertures of increasing radius. The measurement errors account for typical seeing variations during the observations and uncertainties from the PSF shape. Note (8): Intrinsic FWHM size along the major axis, derived from fitting a 1D Gaussian to the Hα light profile taken in 6-pixels-wide circular apertures along the major axis of each galaxy. For some of the sources with faintest Hα surface brightness, major axis profiles are too unreliable for an FWHM determination. The measurement errors account for typical seeing variations during the observations and uncertainties from the PSF shape. Note (9): Fractional contribution of the Hα emission line to the observed broadband flux density (K for sources at 2<z<2.6 and H for those at 1.3<z<2).
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Galaxy name 14 A1 --- l_Lobs Limit flag on lobs 15- 19 F5.2 10+35W Lobs Observed Halpha line luminosity (10) 21- 24 F4.2 10+35W E_Lobs ? Positive error on Lobs 26- 29 F4.2 10+35W e_Lobs ? Negative error on Lobs 31 A1 --- l_L0 Limit flag on L0 32- 36 F5.2 10+35W L0 ? Intrinsic Halpha line luminosity (10) 38- 41 F4.2 10+35W E_L0 ? Positive error on L0 43- 46 F4.2 10+35W e_L0 ? Negative error on L0 48 A1 --- l_L00 Limit flag on L00 49- 54 F6.2 10+35W L00 ? Intrinsic Halpha line luminosity with attenuation (10) 56- 60 F5.1 10+35W E_L00 ? Positive error on L00 62- 66 F5.1 10+35W e_L00 ? Negative error on L00 68- 73 F6.2 10+35W L0p ? Predicted intrinsic Halpha line luminosity from best-fit parameters (11) 75- 80 F6.2 10+35W E_L0p ? Positive error on L0p 82- 86 F5.2 10+35W e_L0p ? Negative error on L0p 88 A1 --- l_Wsin Limit flag on Wsin 89- 92 I4 0.1nm Wsin ? SINFONI Halpha equivalent width (12) 94- 96 I3 0.1nm E_Wsin ? Positive error on Wsin 98-100 I3 0.1nm e_Wsin ? Negative error on Wsin 102 A1 --- l_Wbb Limit flag on Wbb 103-106 I4 0.1nm Wbb ? Halpha equivalent width from the broadband magnitudes (13) 108-110 I3 0.1nm E_Wbb ? Positive error on Wbb 112-114 I3 0.1nm e_Wbb ? Negative error on Wbb 116 A1 --- l_W0bb Limit flag on W0bb 117-120 I4 0.1nm W0bb ? Halpha equivalent width from the broadband magnitudes corrected for extra attenuation (13) 122-124 I3 0.1nm E_W0bb ? Positive error on W0bb 126-128 I3 0.1nm e_W0bb ? Negative error on W0bb 130-132 I3 0.1nm Wp ? Predicted Halpha equivalent width (14) 134-136 I3 0.1nm E_Wp ? Positive error on Wp 138-140 I3 0.1nm e_Wp ? Negative error on Wp
Note (10): Observed and intrinsic Hα line luminosities in 1042erg/s. L0(Hα) is computed assuming the best-fit extinction AV,SED from the SED modeling and the Calzetti et al. (2000ApJ...533..682C) reddening law, and L00(Hα) is computed assuming extra attenuation toward the HII regions with AV,neb=AV,SED/0.44. Uncertainties on the luminosities include the formal 1σ uncertainties of the Hα line fluxes, as well as those of AV from the SED modeling for the intrinsic luminosities; 3σ upper limits are given for sources undetected in Hα. Note (11): Predicted intrinsic Hα line luminosities computed from Bruzual & Charlot (2003MNRAS.344.1000B) models for the best-fit parameters of each galaxy (Table 3). Uncertainties are computed based on those of the best-fit properties derived from the SED modeling. Note (12): Hα equivalent widths from the Hα line fluxes and estimates of the underlying continuum flux density from our SINFONI data. Uncertainties account for the formal 1σ uncertainties on the Hα line fluxes and on the continua; 3σ upper limits are given for sources undetected in Hα, and 3σ lower limits are given for those undetected in the continuum. Note (13): Hα equivalent widths derived from our Hα line flux measurements and estimates of the underlying continuum obtained from the broadband magnitudes (K band for sources at 2<z<2.6 and H for those at 1.3<z<2) after correcting for the contribution by the Hα line (Table 6). The WrestBB(Hα) are computed from the observed Hα fluxes and broadband magnitudes, equivalent to assuming the same extinction applies to the HII regions and the stars. The Wrest,00BB(Hα) are corrected for extra attenuation toward the HII regions, using the best-fit extinction AV,SED from the SED modeling, the Calzetti et al. (2000ApJ...533..682C) reddening law, and applying AV,neb=AV,SED/0.44. Uncertainties account for the formal 1σ uncertainties on the Hα line fluxes and on broadband magnitudes, as well as for the best-fit AV from the SED modeling for Wrest,00BB(Hα); 3σ upper limits are given for sources undetected in Hα. Note (14): Predicted Hα equivalent widths computed from Bruzual & Charlot (2003MNRAS.344.1000B) models for the best-fit parameters of each galaxy (Table 3). Uncertainties are computed based on those of the best-fit properties derived from the SED modeling.
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Source name 14- 19 F6.2 Msun/yr SFRi ? Intrinsic star formation rate from SED 21- 25 F5.1 Msun/yr E_SFRi ? Positive error on SFR (15) 27- 32 F6.2 Msun/yr e_SFRi ? Negative error on SFR (15) 34 A1 --- l_SFR0 Limit flag on SFR0 35- 39 F5.1 Msun/yr SFR0 ? Intrinsic star formation rate derived from the Hα line luminosity (16) 41- 44 F4.1 Msun/yr E_SFR0 ? Positive error in SFR0 46- 49 F4.1 Msun/yr e_SFR0 ? Negative error in SFR0 51 A1 --- l_SFR00 Limit flag on SFR00 52- 57 F6.1 Msun/yr SFR00 ? Intrinsic star formation rate derived from the Hα line luminosity + correction (16) 59- 63 F5.1 Msun/yr E_SFR00 ? Positive error in SFR00 65- 69 F5.1 Msun/yr e_SFR00 ? Negative error in SFR00 71 A1 --- l_LoUV Limit flag on LoUV 72- 75 F4.1 10+21W/Hz LoUV ? Observed UV luminosity density (17) 77- 79 F3.1 10+21W/Hz e_LoUV ? LoUV uncertainty (17) 81 A1 --- l_L0UV Limit flag on L0UV 82- 87 F6.1 10+21W/Hz L0UV ? Intrinsic UV luminosity (17) 89- 93 F5.1 10+21W/Hz E_L0UV ? Positive error in L0UV 95- 99 F5.1 10+21W/Hz e_L0UV ? Negative error in L0UV 101 A1 --- l_SFRuv Limit flag on SFRuv 102-108 F7.2 Msun/yr SFRuv ? Intrinsic star formation rate derived from the rest-frame UV luminosity density (18) 110-115 F6.2 Msun/yr E_SFRuv ? Positive error in SFRuv 117-122 F6.2 Msun/yr e_SFRuv ? Negative error in SFRuv
Note (15): Intrinsic star formation rate corresponding 68% confidence intervals derived from the SED modeling (Table 3). Note (16): Intrinsic star formation rate derived from the Hα line luminosity (see Table 7), applying the conversion of Kennicutt (1998ApJ...498..541K) adjusted to a Chabrier (2003PASP..115..763C) IMF. The SFR0(Hα) are computed assuming the best-fit extinction AV,SED from the SED modeling and the Calzetti et al. (2000ApJ...533..682C) reddening law, and the SFR00(Hα) are computed assuming extra attenuation toward the HII regions with AV,neb=AV,SED/0.44. Uncertainties are propagated from those of the luminosities; 3σ upper limits are given for sources undetected in Hα. Note (17): Observed and intrinsic rest-frame UV luminosity densities in 1028erg/s/Hz, derived from either the B- or G-band magnitude (see Table 2) as described in Section 8.1. The extinction correction uses the best-fit extinction AV,SED from the SED modeling and is computed for a rest-frame wavelength of 1500Å assuming the Calzetti et al. (2000ApJ...533..682C) reddening law. Uncertainties are computed from those of the observed magnitudes, as well as of the best-fit AV from the SED modeling for the intrinsic luminosity; the 3σ upper limit is given for SA15-7353, undetected in the B band. Note (18): Intrinsic star formation rate derived from the rest-frame UV luminosity density, applying the conversion of Kennicutt (1998ApJ...498..541K) adjusted to a Chabrier (2003PASP..115..763C) IMF and corrected for extinction using the best-fit extinction AV,SED from the SED modeling as for the intrinsic rest-frame UV luminosity. Uncertainties are propagated from those of the luminosities; the 3σ upper limit is given for SA15-7353, undetected in the B band.
Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Source name 13 A1 --- f_Name [i] Flag on name (1) 15- 37 A23 --- Met Method used to derive the circular velocity Vel and dynamical mass Mdyn (2) 39- 44 A6 --- Kin Kinemetry class (Disk or Merger) (3) 46- 48 I3 km/s Vel/2 Half the observed velocity (nu_obs_/2) (4) 50- 51 I2 km/s e_Vel/2 Vel/2 uncertainty 53- 56 F4.2 --- V/2sig Rotation- or dispersion-dominated galaxy (5) 58- 61 F4.2 --- E_V/2sig Positive error on V/2sig 63- 66 F4.2 --- e_V/2sig Negative error on V/2sig 68- 70 F3.1 --- Vrot/sig ? Ratio of circular velocity and velocity dispersion (6) 72- 74 F3.1 --- e_Vrot/sig ? Vrot/sig uncertainty 76 A1 --- l_Vel Limit flag on Vel 77- 79 I3 km/s Vel Disk circular velocity (nu_d_) (7) 81- 83 I3 km/s E_Vel ? Positive error on Vel 85- 87 I3 km/s e_Vel ? Negative error on vel 89- 92 F4.2 10+10Msun M0 ? Total gas mass from SFR0 (8) 94- 97 F4.2 10+10Msun E_M0 ? Positive error on M0 99-102 F4.2 10+10Msun e_M0 ? Negative error on M0 104-108 F5.2 10+10Msun M00 ? Total gas mass from SFR00 (8) 110-113 F4.2 10+10Msun E_M00 ? Positive error on M00 115-118 F4.2 10+10Msun e_M00 ? Negative error on M00 120 A1 --- l_Mdyn Limit flag on Mdyn 121-125 F5.2 10+10Msun Mdyn Total dynamical mass 127-131 F5.2 10+10Msun E_Mdyn ? Positive error on Mdyn 133-137 F5.2 10+10Msun e_Mdyn ? Negative error on Mdyn
Note (1): i = This source is classified as (minor) merger from its Hα kinematics, and a small faint close companion is also seen in Hα and continuum emission; the kinematic properties reported here are for the larger main disk component of the system. Note (2): Method used to derive the circular velocity and dynamical mass estimates as explained in Section 9.5. In brief, methods as follows: Kinematic modeling = from full kinematic modeling of the velocity field and velocity dispersion map (Genzel et al. 2008ApJ...687...59G; Cresci et al. 2009ApJ...697..115C). Velocity gradient+width = for sources with rotation-dominated kinematics, the values adopted are averages obtained from estimates based on the observed velocity gradient and on the integrated velocity line width in the framework of rotating disks. Velocity width = for sources with dispersion-dominated kinematics, we used virial isotropic estimates. Galaxies that are undetected in our SINFONI data or for which we cannot establish whether their kinematics are rotation- or dispersion-dominated due to poorer S/N are excluded. Note (3): Classification based on quantitative analysis of the Hα kinematics through kinemetry (see Shapiro et al. 2008ApJ...682..231S, and Section 9.1). Note (4): The νobs is the full observed difference between the maximum and minimum relative velocities from the Hα kinematics across the source, uncorrected for inclination. Note (5): Ratio of half the observed velocity gradient to the source-integrated velocity dispersion (from Table 6), derived from the Hα kinematics and uncorrected for inclination. We treated galaxies with νobs/(2σint)>0.4 as rotation-dominated and those with νobs/(2σint)<0.4 as dispersion-dominated (see Section 9). Note (6): Ratio of inclination-corrected circular velocity and intrinsic local velocity dispersion for the disks with kinematic modeling, corrected for inclination (Genzel et al. 2008ApJ...687...59G; Cresci et al. 2009ApJ...697..115C). Note (7): Disk circular velocity (or equivalent (3σint)0.5 for objects with dispersion-dominated Hα kinematics) derived according to the method given in the second column and described in Section 9.5. Note (8): Total gas masses estimated from the Hα star formation rate surface densities (within the Hα half-light radius r1/2(H{alpha) from Table 6) through the Schmidt-Kennicutt relation as derived by Bouche et al. (2007ApJ...671..303B). Two estimates are listed, depending on the extinction correction applied to the Hα line luminosities: M0gas uses SFR0(Hα) derived using the best-fit extinction AV,SED from the SED modeling (Table 3) and the Calzetti et al. (2000ApJ...533..682C) reddening law, and M00gas uses SFR00(Hα) assuming extra attenuation toward the HII regions with AV,neb=AV,SED/0.44.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode Bibcode 24- 53 A30 --- Aut First author's name 55-103 A49 --- Comm Comment
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 16-Dec-2011
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