CO(1–0) detection of molecular gas in the massive Spiderweb Galaxy (z = 2)★

Emonts, Bjorn; Feain, Ilana; Röttgering, H. J. A.; Miley, G. K.; Seymour, N.; Norris, R. P.; Carilli, Christopher L.; Villar-Martín, M.; Mao, Minnie; Sadler, E. M.; Ekers, R. D.; Moorsel, G. A. van; Ivison, R. J.; Pentericci, L.; Tadhunter, C. N.; Saikia, D. J.

doi:10.1093/mnras/stt147

Cited by 48 publications

(85 citation statements)

References 61 publications

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“…3 left), has a Lorentzian-shaped profile, with a full-width at half-maxima (FWHM) of 270 ± 15 km s −1 and a redshift of z = 2.1606 ± 0.0041, which agrees with the redshift determined from the CO(1-0) line (Emonts et al 2013). We adopt this as the systemic redshift since the [CI]2-1 line has higher spectral resolution and S/N compared to the HeII λ1640 Å (Hatch et al 2008).…”

Section: The Hzrgsupporting

confidence: 76%

“…We find a total H 2 molecular gas mass for both components of 3.3 × 10 10 M . We note that this value depends on the adopted Q 21 : for the highest Q 21 = 1.0, the M(H 2 ) drops to 2.2 × 10 10 M , while for the lowest Q 21 = 0.15, the M(H 2 ) is 1.5 × 10 11 M The median value is close to M(H 2 ) = 6 × 10 10 M that is derived from CO(1-0) (Emonts et al 2013). This total mass of diffuse molecular gas, as probed by the [CI]2-1 emission, is clearly higher than the warm (T > 300 K) molecular gas mass of order 10 7 to 10 9 M (Ogle et al 2012), which suggests an order of magnitude ratio of warm-to-cold molecular gas between 0.1−10%.…”

Section: Mass Estimatesmentioning

confidence: 52%

“…Comparing L CO(7−6) = 1.2 × 10 10 K km s −1 pc 2 with L CO(1−0) = 6.5 × 10 10 K km s −1 pc 2 (Emonts et al 2013), we find that the CO(7-6) emission is only 18% of the value for thermalised gas. This indicates that the molecular gas phase is not thermalised and dominated by the cold and diffuse gas, which is traced by the [CI]2-1 emission line 1 .…”

Section: Possible Causes Of Observed Line Ratiomentioning

confidence: 75%

“…This indicates that the molecular gas phase is not thermalised and dominated by the cold and diffuse gas, which is traced by the [CI]2-1 emission line 1 . Alternatively, a fraction of the CO in the Spiderweb galaxy may be dissociated Röttgering et al (1997) and the CO(1-0) redshift and error (blue bar) from Emonts et al (2013). (2013) by cosmic-rays, increasing the fraction of atomic carbon in the molecular gas without strongly affecting the excitation of [CI]2-1 or the ionisation state of carbon (Bisbas et al 2015).…”

Section: Possible Causes Of Observed Line Ratiomentioning

confidence: 99%

“…Emonts et al (2013) probe the diffuse extended molecular gas reservoir using the CO(1-0) line. They find that there is approximately 6 × 10 10 M of cold H 2 gas over a scale of 10 s of kpc, which surrounds the HzRG (also Emonts et al, in prep.).…”

Section: Introductionmentioning

confidence: 99%

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ALMA finds dew drops in the dusty spider’s web

Gullberg

Lehnert

Breuck

et al. 2016

A&A

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We present 0 . 5 resolution ALMA detections of the observed 246 GHz continuum, [CI] 3 P 2 → 3 P 1 fine structure line ([CI]2-1), CO(7-6), and H 2 O lines in the z = 2.161 radio galaxy MRC1138-262, the so-called Spiderweb galaxy. We detect strong [CI]2-1 emission both at the position of the radio core, and in a second component ∼4 kpc away from it. The 1100 km s −1 broad [CI]2-1 line in this latter component, combined with its H 2 mass of 1.6 × 10 10 M , implies that this emission must come from a compact region <60 pc, possibly containing a second active galactic nucleus (AGN). The combined H 2 mass derived for both objects, using the [CI]2-1 emission, is 3.3 × 10 10 M . The total CO(7-6)/[CI]2-1 line flux ratio of 0.2 suggests a low excitation molecular gas reservoir and/or enhanced atomic carbon in cosmic ray dominated regions. We detect spatially-resolved H 2 O 2 11 −2 02 emission -for the first time in a high-z unlensed galaxy -near the outer radio lobe to the east, and near the bend of the radio jet to the west of the radio galaxy. No underlying 246 GHz continuum emission is seen at either position. We suggest that the H 2 O emission is excited in the cooling region behind slow (10-40 km s −1 ) shocks in dense molecular gas (10 3−5 cm −3 ). The extended water emission is likely evidence of the radio jet's impact on cooling and forming molecules in the post-shocked gas in the halo and inter-cluster gas, similar to what is seen in low-z clusters and other high-z radio galaxies. These observations imply that the passage of the radio jet in the interstellar and inter-cluster medium not only heats gas to high temperatures, as is commonly assumed or found in simulations, but also induces cooling and dissipation, which can lead to substantial amounts of cold dense molecular gas. The formation of molecules and strong dissipation in the halo gas of MRC1138-262 may explain both the extended diffuse molecular gas and the young stars observed around MRC1138-262.

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Section: The Hzrgsupporting

confidence: 76%

Section: Mass Estimatesmentioning

confidence: 52%

Section: Possible Causes Of Observed Line Ratiomentioning

confidence: 75%

Section: Possible Causes Of Observed Line Ratiomentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ALMA finds dew drops in the dusty spider’s web

Gullberg

Lehnert

Breuck

et al. 2016

A&A

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The realm of the galaxy protoclusters

Overzier

2016

Astron Astrophys Rev

262

204

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The study of galaxy protoclusters is beginning to fill in unknown details of the important phase of the assembly of clusters and cluster galaxies. This review describes the current status of this field and highlights promising recent findings related to galaxy formation in the densest regions of the early universe. We discuss the main search techniques and the characteristic properties of protoclusters in observations and simulations, and show that protoclusters will have present-day masses similar to galaxy clusters when fully collapsed. We discuss the physical properties of galaxies in protoclusters, including (proto-)brightest cluster galaxies, and the forming red sequence. We highlight the fact that the most massive halos at high redshift are found in protoclusters, making these objects uniquely suited for testing important recent models of galaxy formation. We show that galaxies in protoclusters should be among the first galaxies at high redshift making the transition from a gas cooling regime dominated by cold streams to a regime dominated by hot intracluster gas, which could be tested observationally. We also discuss the possible connections between protoclusters and radio galaxies, quasars, and Ly-alpha blobs. Because of their early formation, large spatial sizes and high total star formation rates, protoclusters have also likely played a crucial role during the epoch of reionization, which can be tested with future experiments that will map the neutral and ionized cosmic web. Last, we review a number of promising observational projects that are expected to make significant impact in this growing, exciting field.Comment: Invited article for The Astronomy and Astrophysics Review (in press

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Revealing AGN, young and old stellar populations in HzRGs with PEGASE.3

Drouart

Breuck²,

Vernet³

et al. 2013

Proc. IAU

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The HeRGÉ (Herschel Radio Galaxy Evolution) project consists of a sample of 70 radio galaxies in the range 1 < z < 5.2. They benefit from continuous coverage from 3 to 870μm with Spitzer, Herschel and sub-mm ground-based instruments (SCUBA, LABOCA). As a calorimeter, IR is an excellent proxy to estimate the contribution of both AGN and starburst, making of radio galaxies perfect candidates to provide new insights into the relationship between AGN and their host galaxies. The IR SED fitting with empirical templates reveals that radio galaxies are luminous and that their black holes and their host galaxies are not growing simultaneously. Extending the SED to optical/near-IR on a subsample of 12 radio galaxies spanning 1 < z < 4 reveal the necessity of three components to reproduce the observations. Making use of the evolutionary code PEGASE.3 and an AGN torus model, we are able to estimate parameters from the AGN torus, the evolved stellar population and the starburst (SB). They reveal that radio galaxies are massive, evolved, forming the bulk of their mass at very high redshift in a short timescale, but experience episodic, strong SB events, often associated with an AGN activity.

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CO(1–0) detection of molecular gas in the massive Spiderweb Galaxy (z = 2)★

Cited by 48 publications

References 61 publications

ALMA finds dew drops in the dusty spider’s web

ALMA finds dew drops in the dusty spider’s web

The realm of the galaxy protoclusters

Revealing AGN, young and old stellar populations in HzRGs with PEGASE.3

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