J/ApJ/837/40 The MASSIVE survey. VI. Warm ionized gas. (Pandya+, 2017)
The MASSIVE survey.
VI. The spatial distribution and kinematics of warm ionized gas in the most
massive local early-type galaxies.
Pandya V., Greene J.E., Ma C.-P., Veale M., Ene I., Davis T.A.,
Blakeslee J.P., Goulding A.D., McConnell N.J., Nyland K., Thomas J.
<Astrophys. J., 837, 40-40 (2017)>
=2017ApJ...837...40P 2017ApJ...837...40P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Velocity dispersion ; Interstellar medium
Keywords: galaxies: elliptical and lenticular, cD; galaxies: evolution;
galaxies: ISM; galaxies: kinematics and dynamics;
ISM: kinematics and dynamics; ISM: lines and bands
Abstract:
We present the first systematic investigation of the existence,
spatial distribution, and kinematics of warm ionized gas as traced by
the [OII]3727Å emission line in 74 of the most massive galaxies in
the local universe. All of our galaxies have deep integral-field
spectroscopy from the volume- and magnitude-limited MASSIVE survey of
early-type galaxies with stellar mass log(M*/M☉)>11.5
(MK←25.3mag) and distance D<108Mpc. Of the 74 galaxies in our
sample, we detect warm ionized gas in 28, which yields a global
detection fraction of 38±6% down to a typical [OII] equivalent width
limit of 2Å. MASSIVE fast rotators are more likely to have gas than
MASSIVE slow rotators with detection fractions of 80±10% and
28±6%, respectively. The spatial extents span a wide range of radii
(0.6-18.2kpc; 0.1-4Re), and the gas morphologies are diverse, with
17/28∼61±9% being centrally concentrated, 8/28∼29±9% exhibiting
clear rotation out to several kiloparsecs, and 3/28∼11±6% being
extended but patchy. Three out of four fast rotators show kinematic
alignment between the stars and gas, whereas the two slow rotators
with robust kinematic measurements available exhibit kinematic
misalignment. Our inferred warm ionized gas masses are roughly
∼105M☉. The emission line ratios and radial equivalent width
profiles are generally consistent with excitation of the gas by the
old underlying stellar population. We explore different gas origin
scenarios for MASSIVE galaxies and find that a variety of physical
processes are likely at play, including internal gas recycling,
cooling out of the hot gaseous halo, and gas acquired via mergers.
Description:
This paper is based on integral-field spectra obtained with the
Mitchell Spectrograph (formerly VIRUS-P) on the 2.7m Harlan J. Smith
Telescope at McDonald Observatory. The spectra cover the wavelength
range from ∼3500Å to ∼5800Å. We generally have three dithered
pointings for a total of 738 spectra per galaxy.
See the MASSIVE survey description in Paper I: Ma+, 2014, J/ApJ/795/158
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 113 28 Sample of MASSIVE galaxies with warm ionized gas
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See also:
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
J/A+AS/120/257 : Ionized gas velocity in 6 galaxies (Zeilinger+ 1996)
J/ApJS/112/315 : Spectroscopic parameters of Seyfert nuclei (Ho+ 1997)
J/ApJS/127/39 : Stellar & gas kinematics in early-type galaxies (Caon+ 2000)
J/ApJ/655/790 : Groups of galaxies in 2MASS survey (Crook+, 2007)
J/A+A/519/A40 : Spectroscopic study of 65 nearby galaxies (Annibali+, 2010)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/414/888 : ATLAS3D project. III. (Emsellem+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV. (Young+, 2011)
J/ApJS/199/26 : The 2MASS Redshift Survey (2MRS) (Huchra+, 2012)
J/ApJ/795/158 : The MASSIVE survey : 116 candidate galaxies (Ma+, 2014)
J/A+A/573/A111 : Group-dominant elliptical gal. CO spectra (O'Sullivan+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Galaxy name
10- 14 F5.1 Mpc Dist [34/108] Distance taken from Ma+, J/ApJ/795/158
16- 20 F5.2 kpc Reff [2/19] Stellar effective radius
22- 26 F5.2 kpc Rgas [0.6/18.3] Maximum gas radius
28- 33 F6.2 mag KMag [-26.3/-25.4] Absolute K-band AB magnitude
35- 39 F5.2 [Msun] logM* [11.6/12.1] Logarithm of stellar mass
41- 44 F4.1 [Msun] logMd [10/15]? Logarithm of the dark matter halo mass
46- 49 F4.2 [Msun] logMg [3.5/6] Logarithm of the warm ionized
gas mass (1)
51- 54 F4.1 [10-7W] logLHb [37/39.4] Logarithm of Hβ luminosity,
in erg/s units
56- 61 F6.2 km/s sigma [231/354] Central stellar velocity dispersion
63- 63 A1 --- l_OIII/Hb Limit flag on OIII/Hb, if Hβ is
non-detected
65- 68 F4.2 --- OIII/Hb [0.6/5.8] Flux ratio [OIII]/Hβ in the
central spectrum
70- 74 F5.1 deg PAgas [148/357]? Kinematic position angle of
rotating warm ionized gas (2)
76- 79 F4.1 deg e_PAgas [1.6/16.5]? Uncertainty in PAgas
81- 85 F5.1 deg PAstars [1.6/343] Kinematic position angle of
the stars (2)
87- 90 F4.1 deg e_PAstars [0.2/22] Uncertainty in PAstars
92- 92 A1 --- f_PAstars Flag on PAstars (3)
94- 97 F4.1 deg PAdiff [1/98]? Kinematic misalignment angle,
warm ionized gas relative to stars
99-102 F4.1 deg e_PAdiff [3/18]? Uncertainty in PAdiff
104-105 A2 --- F/S Kinematic classification (4)
107-109 A3 --- Ext [Yes/No ] Is warm ionized gas extended beyond
the central three dithered fibers
111-113 A3 --- Rot Does warm ionized gas show regular rotation
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Note (1): The warm ionized gas mass is derived using the Hβ luminosity
according to Equation 1:
MHβ=28.2x108LHβ,43ne,100-1M☉
where LHβ,43 is the Hβ luminosity in units of 1043erg/s
and ne,100 is the electron number density in units of 100cm-3.
See section 4.6.
Note (2): PA is measured counterclockwise from north to the redshifted emission
side.
Note (3): A flag=1 identifies "non-rotators" for which kinemetry was unable
to determine a kinematic stellar position angle; for these galaxies,
their photometric stellar position angles are given instead with an
assumed 10% fractional uncertainty (see subsection 4.4 for details).
Note (4): Kinematic classification as fast or slow rotator from
Veale+ (2017MNRAS.464..356V 2017MNRAS.464..356V) based on angular momentum within Reff.
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History:
From electronic version of the journal
References:
Ma et al. Paper I. 2014ApJ...795..158M 2014ApJ...795..158M Cat. J/ApJ/795/158
Green et al. Paper II. 2015ApJ...807...11G 2015ApJ...807...11G
Davis et al. Paper III. 2016MNRAS.455..214D 2016MNRAS.455..214D
Goulding et al. Paper IV. 2016ApJ...826..167G 2016ApJ...826..167G
Veale et al. Paper V. 2017MNRAS.464..356V 2017MNRAS.464..356V
Pandya et al. Paper VI. 2017ApJ...837...40P 2017ApJ...837...40P This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Oct-2017