J/ApJ/899/13 GASP. XXI. Star forming rate in 54 galaxies (Gullieuszik+, 2020)
GASP.
XXI. Star Formation Rates in the Tails of Galaxies Undergoing Ram Pressure
Stripping.
Gullieuszik M., Poggianti B.M., McGee S.L., Moretti A., Vulcani B.,
Tonnesen S., Roediger E., Jaffe Y.L., Fritz J., Franchetto A., Omizzolo A.,
Bettoni D., Radovich M., Wolter A.
<Astrophys. J., 899, 13 (2020)>
=2020ApJ...899...13G 2020ApJ...899...13G
ADC_Keywords: Galaxies; Redshifts; Velocity dispersion; Star Forming Region;
Optical
Keywords: Galaxy evolution ; Ram pressure stripped tails
Abstract:
Using MUSE observations from the GASP survey, we study 54 galaxies
undergoing ram pressure stripping (RPS) and spanning a wide range in
galaxy mass and host cluster mass. We use this rich sample to study
how the star formation rate (SFR) in the tails of stripped gas depends
on the properties of the galaxy and its host cluster. We show that the
interplay between all the parameters involved is complex and that
there is not a single, dominant one in shaping the observed amount of
SFR. Hence, we develop a simple analytical approach to describe the
mass fraction of stripped gas and the SFR in the tail, as a function
of the cluster velocity dispersion, galaxy stellar mass,
clustercentric distance, and speed in the intracluster medium. Our
model provides a good description of the observed gas truncation
radius and of the fraction of SFR observed in the stripped tails, once
we take into account the fact that the star formation efficiency in
the tails is a factor of ∼5 lower than in the galaxy disk, in
agreement with GASP ongoing HI and CO observations. Finally, we
estimate the contribution of RPS to the intracluster light (ICL) and
find that the average SFR in the tails of ram pressure stripped gas is
∼0.22M☉/yr per cluster. By extrapolating this result to evaluate
the contribution to the ICL at different epochs, we compute an
integrated average value per cluster of ∼4x109M☉ of stars formed
in the tails of RPS galaxies since z∼1.
Description:
GAs Stripping Phenomena (GASP) observations were carried out between
2015 October and 2018 April in service mode with the Multi Unit
Spectroscopic Explorer (MUSE) integral-field spectrograph mounted at
the Nasmyth focus of the UT4 Very Large Telescope (VLT), at Cerro
Paranal in Chile. The MUSE spectral range, between 4500 and 9300Å,
is sampled at 1.25Å/pixel, with a spectral resolution of ∼2.6Å.
The 1x1' field of view (FoV) is sampled at 0.2"/pixel.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 79 54 Properties of GASP galaxies used in this work
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See also:
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/MNRAS/416/727 : Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)
J/A+A/587/A68 : Ionised gas images of NGC 4569 (Boselli+, 2016)
J/AJ/151/78 : Jellyfish galaxy cand. in galaxy clusters (Poggianti+, 2016)
J/A+A/607/A81 : Properties of the sample of clusters (Biviano+, 2017)
J/A+A/599/A81 : OmegaWINGS clusters of galaxies redshifts (Moretti+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- ID GASP ID number (1)
7- 8 I2 h RAh [0/23] Hour of Right Ascension (J2000)
10- 11 I2 min RAm Minute of Right Ascension (J2000)
13- 17 F5.2 s RAs Second of Right Ascension (J2000)
19- 19 A1 --- DE- [±] Sign of the Declination (J2000)
20- 21 I2 deg DEd Degree of Declination (J2000)
23- 24 I2 arcmin DEm Arcminute of Declination (J2000)
26- 29 F4.1 arcsec DEs Arcsecond of Declination (J2000)
31- 37 A7 --- Cluster Host cluster
39- 42 I4 km/s sigmaCl [387/1147] Velocity dispersion of the host
cluster
44- 48 F5.2 [Msun] [Mass] [8.76/11.5] logarithm of the galaxy stellar
mass
50- 55 F6.4 --- z [0.035/0.073] galaxy redshift
57- 61 F5.3 solMass/yr SFRtot [0.11/8.45] total star formation rate
63- 67 F5.3 solMass/yr SFRout [0/1.14] star formation rate in the tails
69- 72 F4.2 --- rcl/r200 [0.06/1.73] projected distance from the
cluster centre in units of R200
74- 77 F4.2 --- v/sigmaCL [0/3.66] line of sight velocity of the
galaxy with respect to the cluster mean in
units of the cluster velocity dispersion
79- 79 I1 --- JC [1/5] Jellyfish Class (JC) (1)
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Note (1): Identifier and class from Poggianti+, 2016, J/AJ/151/78
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History:
From electronic version of the journal
References:
Poggianti et al. Paper I : 2017ApJ...844...48P 2017ApJ...844...48P
Bellhouse et al. Paper II : 2017ApJ...844...49B 2017ApJ...844...49B
Fritz et al. Paper III : 2017ApJ...848..132F 2017ApJ...848..132F
Gullieuszik et al. Paper IV : 2017ApJ...846...27G 2017ApJ...846...27G
Moretti et al. Paper V : 2018MNRAS.475.4055M 2018MNRAS.475.4055M
Vulcani et al. Paper VII : 2018ApJ...852...94V 2018ApJ...852...94V
Vulcani et al. Paper VIII : 2017ApJ...850..163V 2017ApJ...850..163V
Jaffe et al. Paper IX : 2018MNRAS.476.4753J 2018MNRAS.476.4753J
Moretti et al. Paper X : 2018MNRAS.480.2508M 2018MNRAS.480.2508M
Vulcani et al. Paper XII : 2018MNRAS.480.3152V 2018MNRAS.480.3152V
Poggianti et al. Paper XIII : 2019MNRAS.482.4466P 2019MNRAS.482.4466P
Bellhouse et al. Paper XV : 2019MNRAS.485.1157B 2019MNRAS.485.1157B
Vulcani et al. Paper XVI : 2019MNRAS.487.2278V 2019MNRAS.487.2278V
Ramatsoku et al. Paper XVII : 2019MNRAS.487.4580R 2019MNRAS.487.4580R
George et al. Paper XVIII : 2019MNRAS.487.3102G 2019MNRAS.487.3102G
Radovich et al. Paper XIX : 2019MNRAS.486..486R 2019MNRAS.486..486R
Vulcani et al. Paper XX : 2019MNRAS.488.1597V 2019MNRAS.488.1597V
Moretti et al. Paper XXII : 2020ApJ...889....9M 2020ApJ...889....9M
Poggianti et al. Paper XXIII : 2019ApJ...887..155P 2019ApJ...887..155P
Vulcani et al. Paper XXIV : 2020ApJ...892..146V 2020ApJ...892..146V
Deb et al. Paper XXV : 2020MNRAS.494.5029D 2020MNRAS.494.5029D
Ramatsoku et al. Paper XXVI : 2020A&A...640A..22R 2020A&A...640A..22R
Franchetto et al. Paper XXVIII : 2020ApJ...895..106F 2020ApJ...895..106F Cat. J/ApJ/895/106
Bellhouse et al. Paper XXIX : 2021MNRAS.500.1285B 2021MNRAS.500.1285B
Vulcani et al. Paper XXX : 2020ApJ...899...98V 2020ApJ...899...98V
Tomicic et al. Paper XXXII : 2021ApJ...907...22T 2021ApJ...907...22T
Vulcani et al. Paper XXXIII : 2021ApJ...914...27V 2021ApJ...914...27V
Campitiello et al. Paper XXXIV : 2021ApJ...911..144C 2021ApJ...911..144C
(End) Prepared by [AAS], Coralie Fix [CDS], 08-Oct-2021