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 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 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 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 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 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 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 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 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 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 2003MNRAS.344.1000B) models with
solar metallicity, the Chabrier (2003PASP..115..763C 2003PASP..115..763C) IMF, and the
Calzetti et al. (2000ApJ...533..682C 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 Hα flux in 10-17erg/s/cm2 (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 Hα 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 Hα
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 Hα 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 Hα 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 Hα 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 Hα 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 Hα 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 ? Hα 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 ? Hα 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 Hα 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 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 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 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 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 1998ApJ...498..541K) adjusted to a Chabrier (2003PASP..115..763C 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 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 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 1998ApJ...498..541K) adjusted to a Chabrier (2003PASP..115..763C 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 (νobs/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 (νd) (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 2008ApJ...687...59G; Cresci et al. 2009ApJ...697..115C 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 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 2008ApJ...687...59G; Cresci
et al. 2009ApJ...697..115C 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 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 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