Merger driven star-formation activity in Cl J1449+0856 at z=1.99 as seen by ALMA and JVLA

Coogan, R. T.; Daddi, E.; Sargent, M.; Strazzullo, V.; Valentino, F.; Gobat, R.; Magdis, G.; Béthermin, M.; Pannella, M.; Onodera, Makoto; Liu, Daizhong; Cimatti, A.; Dannerbauer, H.; Carollo, M.; Renzini, A.; Tremou, Evangelia

doi:10.1093/mnras/sty1446

Cited by 41 publications

(40 citation statements)

References 78 publications

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“…That the environmental quenching efficiency for lower-M * declines rapidly over this window perhaps suggests a similar decline for higher-M * at even higher redshifts than are studied here. Such a picture is consistent with several works studying clusters at z > ∼ 1.4, in which the average star formation is seen in many cases to be unperturbed or even enhanced relative to field environments (e.g., Brodwin et al 2013;Alberts et al 2014Alberts et al , 2016Santos et al 2014;Wang et al 2016;Stach et al 2017;Coogan et al 2018).…”

Section: Environmental Quenching Efficiencysupporting

confidence: 91%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼5000 spectroscopically-confirmed galaxies drawn from the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey we investigate the relationship between color and galaxy density for galaxy populations of various stellar masses in the redshift range 0.55 ≤ z ≤ 1.4. The fraction of galaxies with colors consistent with no ongoing star formation ( f q ) is broadly observed to increase with increasing stellar mass, increasing galaxy density, and decreasing redshift, with clear differences observed in f q between field and group/cluster galaxies at the highest redshifts studied. We use a semi-empirical model to generate a suite of mock group/cluster galaxies unaffected by environmentally-specific processes and compare these galaxies at fixed stellar mass and redshift to observed populations to constrain the efficiency of environmentally-driven quenching (Ψ convert ). High-density environments from 0.55 ≤ z ≤ 1.4 appear capable of efficiently quenching galaxies with log(M * /M ⊙ ) > 10.45. Lower stellar mass galaxies also appear efficiently quenched at the lowest redshifts studied here, but this quenching efficiency is seen to drop precipitously with increasing redshift. Quenching efficiencies, combined with simulated group/cluster accretion histories and results on the star formation rate-density relation from a companion ORELSE study, are used to constrain the average time from group/cluster accretion to quiescence and the elapsed time between accretion and the inception of the quenching event. These timescales were constrained to be t convert = 2.4 ± 0.3 and t delay = 1.3 ± 0.4 Gyr, respectively, for galaxies with log(M * /M ⊙ ) > 10.45 and t convert = 3.3 ± 0.3 and t delay = 2.2 ± 0.4 Gyr for lower stellar mass galaxies. These quenching efficiencies and associated timescales are used to rule out certain environmental mechanisms as being the primary processes responsible for transforming the star-formation properties of galaxies over this 4 Gyr window in cosmic time.

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Section: Environmental Quenching Efficiencysupporting

confidence: 91%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The authors speculated that the environment of galaxy clusters helps feeding the gas through into the cluster members and reduces the efficiency of star formation. On the other hand, Coogan et al (2018) found lower τ H2 , enhanced SFE and highly excited CO SLEDs in protocluster members at z = 1.99, linking such activity to mergers. The general picture of how dense environments might or not contribute to enhance or suppress the accretion of gas and affect its efficiency to form stars is still debated and unclear.…”

Section: Gas Fractions and Star Formation Efficienciesmentioning

confidence: 88%

“…At z ∼ 1.5-2.5 several works have studied the molecular gas content, efficiency of converting gas into stars and their relation with the specific star formation rate (sSFR = SFR/M * ) and with field galaxies, those that do not necessarily live in an overdense environment (e.g., Noble et al 2017;Lee et al 2017;Rudnick et al 2017;Dannerbauer et al 2017;Hayashi et al 2018;Coogan et al 2018). In this section we explore and discuss these matters regarding our sample of protoclusters cores.…”

Section: Gas Fractions and Star Formation Efficienciesmentioning

confidence: 99%

Confirming Herschel Candidate Protoclusters from ALMA/VLA CO Observations

Gómez-Guijarro

Riechers

Pavesi

et al. 2019

ApJ

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ALMA 870 µm continuum imaging has uncovered a population of blends of multiple dusty starforming galaxies (DSFGs) in sources originally detected with the Herschel Space Observatory. However, their pairwise separations are much smaller that what is found by ALMA follow-up of other single-dish surveys or expected from theoretical simulations. Using ALMA and VLA, we have targeted three of these systems to confirm whether the multiple 870 µm continuum sources lie at the same redshift, successfully detecting 12 CO(J = 3-2) and 12 CO(J = 1-0) lines and being able to confirm that in the three cases all the multiple DSFGs are likely physically associated within the same structure. Therefore, we report the discovery of two new gas-rich dusty protocluster cores (HELAISS02, z = 2.171 ± 0.004; HXMM20, z = 2.602 ± 0.002). The third target is located in the well known COSMOS overdensity at z = 2.51 (named CL J1001+0220 in the literature), for which we do not find any new secure CO(1-0) detection, although some of its members show only tentative detections and require further confirmation. From the gas, dust, and stellar properties of the two new protocluster cores, we find very large molecular gas fractions yet low stellar masses, pushing the sources above the main sequence, while not enhancing their star formation efficiency. We suggest that the sources might be newly formed galaxies migrating to the main sequence. The properties of the three systems compared to each other and to field galaxies may suggest a different evolutionary stage between systems.

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“…More details about these ancillary data can be found in Strazzullo et al (2013), Valentino et al (2015Valentino et al ( , 2016, Coogan et al (2018), and references therein.…”

Section: Ancillary Datamentioning

confidence: 99%

A contribution of star-forming clumps and accreting satellites to the mass assembly of z ∼ 2 galaxies

Zanella

Floc’h

Harrison

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analysed spatially resolved HubbleSpace Telescope observations (imaging and slitless spectroscopy) of 53 star-forming galaxies at z ∼ 1–3. We created continuum and emission line maps and pinpointed residual ‘blobs’ detected after subtracting the galaxy disc. Those were separated into compact (unresolved) and extended (resolved) components. Extended components have sizes ∼2 kpc and comparable stellar mass and age as the galaxy discs, whereas the compact components are 1.5 dex less massive and 0.4 dex younger than the discs. Furthermore, the extended blobs are typically found at larger distances from the galaxy barycentre than the compact ones. Prompted by these observations and by the comparison with simulations, we suggest that compact blobs are in situ formed clumps, whereas the extended ones are accreting satellites. Clumps and satellites enclose, respectively, ∼20 per cent and ≲80 per cent of the galaxy stellar mass, ∼30 per cent and ∼20 per cent of its star formation rate. Considering the compact blobs, we statistically estimated that massive clumps (M⋆ ≳ 109 M⊙) have lifetimes of ∼650 Myr, and the less massive ones (108 < M⋆ < 109 M⊙) of ∼145 Myr. This supports simulations predicting long-lived clumps (lifetime ≳ 100 Myr). Finally, ≲30 per cent (13 per cent) of our sample galaxies are undergoing single (multiple) merger(s), they have a projected separation ≲10 kpc, and the typical mass ratio of our satellites is 1:5 (but ranges between 1:10 and 1:1), in agreement with literature results for close pair galaxies.

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Merger driven star-formation activity in Cl J1449+0856 at z=1.99 as seen by ALMA and JVLA

Cited by 41 publications

References 78 publications

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Confirming Herschel Candidate Protoclusters from ALMA/VLA CO Observations

A contribution of star-forming clumps and accreting satellites to the mass assembly of z ∼ 2 galaxies

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