the gasp survey: sf in galaxies undergoing rps · 2019. 11. 14. · gasp. iv. a muse view of...

The GASP survey: SF in galaxies undergoing RPSMarco Gullieuszik

Marco Gullieuszik Galaxy Evolution and Environment 6 Trieste - 28-31.10.2019

This project has received funding from the European Research Council (ERC) under the Horizon 2020 research and innovation programme (ERC Advanced Grant, grant agreement N. 833824)

B. M. Poggianti, PI (INAF-OAPd)

D. Bettoni (INAF-OAPd) A. Biviano (INAF-OAPd)M. Gitti (UniBo)M. Gullieuszik (INAF-OAPd)A. Franchetto (UniPD,INAF-OAPd)A. Ignesti (UniBo)M. Mingozzi (INAF-OAPd)A. Moretti (INAF-OAPd) A. Omizzolo (INAF-OAPd, Specola Vaticana) R. Paladino (INAF-IRA) M. Ramatsoku (INAF-OAC)M. Radovich (INAF-OAPd)P. Serra (INAF-OAC) N. Tomicic (INAF-OAPd)B. Vulcani (INAF-OAPd)A. Wolter (INAF-OAB)

C. Bellhouse (Univ. Birmingham, UK)T. Deb (Kapteyn Astronomical Inst., NL)J. Fritz (IRyA, UNAM, Mexico) K. George (LMU, Germany) G. Hau (ESO, Chile)Y. Jaffé (Univ. de Valparaiso, Chile)S. McGee (Univ. of Birmingham, UK) E. Roediger (University of Hull, UK)S. Tonnesen (CCA, USA)J. van Gorkom (Columbia University, USA) M. Verheijen (Kapteyn Astronomical Inst., NL)

GASP - The Team

GAs Stripping Phenomena in galaxies


The gas cycle

From http://www.spica-mission.org/science_galaxies.xhtml

The primary role of the gas component in galaxy evolution:

Isolated galaxies are self regulating systems+ gas replenishment- consumption (stellar evolution) - Ejection (SN/massive stars/AGN

outflows


The gas cycle: environmental effects

Environmental mechanisms can break the cycle and/or strip gas

> dramatic consequences on galaxy evolution

○ ellipticals● SoＸ Spirals + Irr

LOCAL DENSITY OF GALAXIES

FRA

CTI

ON

OF

PO

PU

LATI

ON

Dressler+1980


The gas cycle: environmental effects

Environmental mechanisms can break the cycle and/or strip gas

> dramatic consequences on galaxy evolution

Ram-pressure stripping Interaction IntraCluster Medium - gas in the galaxy discthe most efficient stripping mechanism in clusters


Ram - pressure stripping galaxies

ionized gas with IFU. Merluzzi+2012

VLA HI. Kenney+2004

ionized gas. MUSE. Fumagalli+2014

Xray . ChandraSun+2010


Ram - pressure stripping galaxies

ionized gas with IFU. Merluzzi+2012

VLA HI. Kenney+2004

ionized gas. MUSE. Fumagalli+2014

Xray . ChandraSun+2010

systematic search for RPS galaxies

Mc Partland+2016massive clusters @ z=0.3 - 0.7

based on HST imaging

Poggianti+2016z=0.04-0.07

based on ground based [Omega]WINGS imaging


GASP - The sample

GAs Stripping Phenomena in galaxies with MUSE

114 galaxies at z~0.05● 64 stripping candidates from Poggianti+2016● 12 control sample cluster galaxies● 38 galaxies in low-density environments

➔ Stellar mass: 109 1011.5 Msun

➔ Host halo mass: 1011 1015.5 Msun (field, groups, clusters)

➔ different stages of stripping to sample the whole stripping history


GASP - multiwavelength observations

Stellar component / ionized gas

CO

HI

ongoing Star Formation

Magnetic fields

hot gas + ICM

(AGN)

120 hours on MUSE/VLT

77 hours on SHFI/APEX22 hours on ALMA (CO)

100 hours on JVLA13 hours on Meerkat

104.4 ks on UVIT/Astrosat. FUV - NUV

50 hours on JVLA

X-ray XMM/Chandra archival data

Xshooter


GASP. I. Gas stripping phenomena in galaxies with MUSEPoggianti et al. (2017a), ApJ 844, 48

GASP. II. A MUSE view of extreme ram-pressure stripping along the line of sight: kinematics of the jellyfish galaxy JO201

Bellhouse et al. (2017), ApJ 844, 49GASP. III. JO36: a case of multiple environmental effects at play?

Fritz et al. (2017), ApJ 848, 132GASP. IV. A Muse View of Extreme Ram-pressure Stripping in the Plane of the Sky: The Case of Jellyfish Galaxy JO204

Gullieuszik et al. (2017), ApJ 846, 27GASP. V. Ram-pressure stripping of a ring Hoag's-like galaxy in a massive cluster

Moretti et al. (2018), MNRAS, 475, 4055 Ram-pressure feeding of supermassive black holes

Poggianti et al. (2017b), Nature, 548, 304GASP. VII. Signs of gas inflow onto a lopsided galaxy

Vulcani et al. (2018a), ApJ 852, 94GASP. VIII. Capturing the birth of a Tidal Dwarf Galaxy in a merging system at z~0.05

Vulcani et al. (2017), ApJ 850, 163GASP IX. Jellyfish galaxies in phase-space: an orbital study of intense ram-pressure stripping in clusters

Jaffé et al. (2018), MNRAS 476, 4753GASP. X: APEX detection of molecular gas in the tails and in the disks of ram-pressure stripped galaxies

Moretti et al. (2018), MNRAS 480, 2508UVIT view of ram-pressure stripping in action: Star formation in the stripped gas of the GASP jellyfish galaxy JO201 in Abell 85

George et al. (2018), MNRAS 479, 4126GASP. XII. The variety of physical processes occurring in a single galaxy group in formation

Vulcani et al. (2018), MNRAS, 480, 3152

GASP. XIII. Star formation in gas outside galaxiesPoggianti et al. (2018), MNRAS, 482, 4466

Enhanced star formation in both disks and ram pressure stripped tails of GASP jellyfish galaxies

Vulcani et al. (2018), ApJ, 866L, 25GASP. XV. A MUSE View of Extreme Ram-Pressure Stripping along the Line of Sight: Physical properties of the Jellyfish Galaxy JO201

Bellhouse et al. (2019), MNRAS, 485, 1157GASP. XVI. Does cosmic web enhancement turn on star formation in galaxies?

Vulcani et al. (2019), MNRAS, 487, 2278GASP. XVII. HI imaging of the jellyfish galaxy JO206: gas stripping and enhanced star formation

Ramatsoku et al. (2019), MNRAS,487, 4580GASP XVIII: Star formation quenching due to AGN feedback in the central region of a jellyfish galaxy

George et al. (2019), MNRAS, 487, 3102GASP - XIX. AGN and their outflows at the centre of jellyfish galaxies

Radovich et al. (2019), MNRAS, 486, 486GASP. XX. From the loose spatially-resolved to the tight global SFR-Mass relation in local spiral galaxies

Vulcani et al. (2019), MNRAS, 488, 1597GASP XXI. Star formation rates in the tails of galaxies undergoing ram-pressure stripping

Gullieuszik et al., ApJ submittedGASP. XXII. The molecular gas content of the JW100 jellyfish galaxy at z∼0.05: does ram pressure promote molecular gas formation?

Moretti at al., ApJ submittedGASP XXIII. A jellyfish galaxy as an astrophysical laboratory of the baryonic cycle

Poggianti et al., ApJ submittedGASP XXIV. Neutral Hydrogen gas in the striking Jellyfish Galaxy JO204

Deb et al. ApJ submitted

GASP - Papers




























GASP - The Survey : observations & methods




























GASP - individual galaxies with MUSE




























GASP - individual galaxies - multi-wavelength




























GASP - physical processes in low mass haloes




























GASP - AGNs




























GASP - General properties of RPS galaxies




























GASP - RPS & SF


GASP - SF Enhanced in RPS galaxy discs

working on spatially resolved SMR-M relation in RPS galaxies>> to be compared with the results on undisturbed galaxies (GASP XX, Vulcani+2019)

Vulcani + 2018


GASP - SF in gas outside RPS galaxies

Poggianti + 2019

● Galaxies with long extraplanar Halpha tails (20-100 kpc long)

● The gas in the tail is ionized by photo-ionization by young massive stars

● The SF take place in bright, dynamically cold (σ=27 km/s ) Hα clumps

● The luminosity of Hα clumps is typical of giant (Carina Nebula) and supergiant (30Dor) HII regions

● The median stellar mass in the clump is 3x106 Msun


SFR in the tails of RPS galaxies

● Measure the SFR in the tails of RPS galaxies

● How does this depends on galaxy and environmental properties?○ galaxy mass○ cluster mass○ velocity in the ICM○ position in the cluster

● what is the contribution to the ICM and ICL?

Sample: all 54 GASP galaxies in clusters. Mergers/interacting galaxies excluded

Gullieuszik + ApJ submitted


SFR in the tails: Sample properties

Galaxy stellar mass

SFR in the tails

host cluster velocity dispersion


SFR in the tails: observational results


SFR in the tails: observational results

The interplay between all the parameters involved is complex

galaxy mass cluster vel dispersion velocity in the ICM cluster-centric distance

There is not a single, dominant one in shaping the amount of SFR observed in the tails


SFR in the tails: analytical model

based on standard Gunn&Gott prescriptions for ram-pressure

● exponential disc profile for gas and stellar components● the gas-to-stellar scale length ratio is 1.7

host cluster:● Beta-model● central density and core-radius are linear functions of cluster mass (ref values from Jaffe+2018)

galaxy:● gas fraction and disc scale-length are functions of galaxy stellar mass (ref values from Jaffe+2018)

=

as a function of


SFR in the tails: analytical model

IF both the star formation efficiency and the fraction of molecular gas, which is the gas phase actively involved in the star formation process, are constant

Observed

model


SFR in the tails: observed vs model

The model provide a good agreement with our data once we adopt k~5

> SF efficiency in the tails is a factor ~5 lower than in the disc

in agreement with ongoing GASP observations of ➔ HI (Ramatsoku+2019, Ramatsoku+ in prep)➔ CO (Moretti+2018, Moretti+ submitted)


contribution to the ICM

Using the whole sample of RPS candidates in Poggianti+2016 to normalize the integrated SFR in the tail we find that the average SFR in the tails of ram-pressure stripped gas is ∼0.22 Msun/yr per cluster

using infalling rate of galaxies in clusters computed from N-body simulations we compute an integrated average value per cluster of ∼4×109 Msun of stars formed in the tails of RPS galaxies since z~1

the gasp survey: sf in galaxies undergoing rps · 2019. 11. 14. · gasp. iv. a muse view of...

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