J/MNRAS/482/2166 Tully-Fisher relation across 8Gyr since z∼1 (Tiley+, 2019)
KROSS-SAMI: a direct IFS comparison of the Tully-Fisher relation across 8 Gyr
since z~=1.
Tiley A.L., Bureau M., Cortese L., Harrison C.M., Johnson H.L., Stott J.P.,
Swinbank A.M., Smail I., Sobral D., Bunker A.J., Glazebrook K., Bower R.G.,
Obreschkow D., Bryant J.J., Jarvis M.J., Bland-Hawthorn J., Magdis G.,
Medling A.M., Sweet S.M., Tonini C., Turner O.J., Sharples R.M.,
Croom S.M., Goodwin M., Konstantopoulos I.S., Lorente N.P.F.,
Lawrence J.S., Mould J., Owers M.S., Richards S.N.
<Mon. Not. R. Astron. Soc., 482, 2166-2188 (2019)>
=2019MNRAS.482.2166T 2019MNRAS.482.2166T (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Rotational velocities ; Redshifts
Keywords: galaxies: evolution - galaxies: general -
galaxies: kinematics and dynamics -
galaxies: star formation
Abstract:
We construct Tully-Fisher relations (TFRs), from large samples of
galaxies with spatially resolved Hα emission maps from the
K-band Multi-Object Spectrograph (KMOS) Redshift One Spectroscopic
Survey (KROSS) at z∼1. We compare these to data from the
Sydney-Australian-Astronomical-Observatory Multi-object Integral-Field
Spectrograph (SAMI) Galaxy Survey at z∼0. We stringently match the
data quality of the latter to the former, and apply identical analysis
methods and sub-sample selection criteria to both to conduct a direct
comparison of the absolute K-band magnitude and stellar mass TFRs at
z∼1 and 0. We find that matching the quality of the SAMI data to that
of KROSS results in TFRs that differ significantly in slope,
zero-point, and (sometimes) scatter in comparison to the corresponding
original SAMI relations. These differences are in every case as large
as or larger than the differences between the KROSS z∼1 and matched
SAMI z∼0 relations. Accounting for these differences, we compare the
TFRs at z∼1 and 0. For disc-like, star-forming galaxies we find no
significant difference in the TFR zero-points between the two epochs.
This suggests the growth of stellar mass and dark matter in these
types of galaxies is intimately linked over this ∼8Gyr period.
Description:
The z∼1 TFRs presented in this work are constructed from samples drawn
from KROSS. For detailed descriptions of the KROSS sample selection,
observations, and data reduction, see Stott et al.
(2016MNRAS.457.1888S 2016MNRAS.457.1888S). KROSS comprises integral field unit (IFU)
observations of 795 galaxies at 0.6~<z~<1, that target Hα,
[NII]6548, and [NII]6583 emission from warm ionized gas that falls in
the YJ band (∼1.02-1.36µm) of KMOS. All KROSS observations were
carried out with KMOS on UT1 of the Very Large Telescope, Cerro
Paranal, Chile. The core KROSS observations were undertaken during ESO
observing periods P92-P95 (with programme IDs 092.B-0538, 093.B-0106,
094.B-0061, and 095.B-0035).
The z∼0 TFRs presented in this work are constructed from samples drawn
from the SAMI Galaxy Survey (Bryant et al. 2015MNRAS.447.2857B 2015MNRAS.447.2857B). Using
the SAMI spectrograph (Croom et al. 2012MNRAS.421..872C 2012MNRAS.421..872C) on the 3.9-m
Anglo-Australian Telescope at Siding Spring Observatory. The SAMI
Galaxy Survey has observed the spatially resolved stellar and gas
kinematics of ∼3000 galaxies in the redshift range 0.004<z<0.095, over
a large range of local environments. This work uses SAMI observations
of 824 galaxies with mapped kinematics out to or beyond one effective
radius.
In this work, we take steps to remove the potential for systematic
biases between TFRs constructed at different redshifts by implementing
a novel data 'matching' process, applied to the SAMI data to transform
them so that they match the quality of KROSS observations. As stated
in Introduction, we refer to these transformed data as the matched
SAMI sample. Table A1 presents examples of the derived values from the
KROSS, original SAMI, and matched SAMI rot-dom and disky galaxy
sub-samples, that were used to construct the TFRs.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 89 754 The derived properties used to construct the
KROSS, original SAMI, and matched SAMI TFRs
for the rot-dom and disky sub-samples
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See also:
J/MNRAS/467/1965 : KMOS Redshift One Spectroscopic Survey (Harrison+, 2017)
J/MNRAS/474/5076 : KMOS Redshift One Spectroscopic Survey (Johnson+, 2018)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Survey The source survey for the galaxy
(KROSS, SAMI_matched or SAMI_original)
15- 20 I6 --- ID The object ID for the corresponding survey
for KROSS survey, KROSS NNNNNN in Simbad
22 I1 --- f_ID [0/1] Flag indicating to which sub-sample(s)
the galaxy belongs (1)
24- 40 F17.15 [km/s] logv2.2 Intrinsic rotation velocity (2)
42- 62 E21.19 [km/s] e_logv2.2 Error on logv2.2 (2)
64- 71 F8.5 [Msun] logMstar The stellar mass derived via SED fitting with
LEPHARE (3)
73- 75 F3.1 [Msun] e_logMstar Error on logMstar (3)
77- 83 F7.3 mag KMAG Absolute K-band magnitude in the Vega system
85- 89 F5.3 mag e_KMAG Error on KMAG
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Note (1): Flag as follows:
0 = the galaxy only belongs to the rot-dom sub-sample
1 = the galaxy belongs to both the rot-dom and disky sub-samples
Note (2): For a unique measure of the intrinsic circular velocity for each
galaxy, we adopt the v2.2 parameter of Harrison et al.
(2017MNRAS.467.1965H 2017MNRAS.467.1965H, Cat. J/MNRAS/467/1965) derived from v2.2,obs,
the line-of-sight velocity measured from the best-fitting model to the
rotation curve at 1.3 times the effective (half-light) radius re
(convolved to the 'native' seeing of the velocity maps). This radius
corresponds to 2.2 times the scale length of a purely exponential
disc.
The KROSS measurements of logv2.2 (and e_logv2.2) are taken directly
from Harrison et al. (2017MNRAS.467.1965H 2017MNRAS.467.1965H, Cat. J/MNRAS/467/1965).
Note (3): The model SEDs were generated using the population synthesis models
of Bruzual & Charlot (2003MNRAS.344.1000B 2003MNRAS.344.1000B). The LEPHARE routine fits
for extinction, metallicity, age, star formation, and stellar mass,
and allows for single burst, exponential decline, and constant star
formation histories.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 27-Jun-2022