Super

Cicone, C.; Mainieri, V.; Circosta, C.; Kakkad, D.; Vietri, G.; Perna, M.; Bischetti, M.; Carniani, Stefano; Cresci, G.; Harrison, C. M.; Mannucci, F.; Marconi, A.; Piconcelli, E.; Puglisi, A.; Scholtz, J.; Vignali, C.; Zamorani, G.; Zappacosta, L.; Battaia, Fabrizio Arrigoni

doi:10.1051/0004-6361/202141611

Cited by 24 publications

(18 citation statements)

References 34 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…An alternative, although unlikely, explanation to the observed properties might be the presence of large-scale molecular gas in the circumgalactic medium, as observed in some other protoclusters (Emonts et al 2016;Ginolfi et al 2017), and also in isolated quasars (see Cicone et al 2021). It is also possible that these massive, extended, and poorly excited molecular gas reservoirs are due to the combined emission of multiple galaxies at similar redshifts (with the low excitation caused by the decreasing beam size in EMIR at increasing frequencies).…”

Section: The Molecular Gas Properties Of the Phz-iram Sourcesmentioning

confidence: 90%

Molecular gas properties of Planck-selected protocluster candidates at z~1.3-3

Polletta,

Dole,

Martinache

et al. 2022

Preprint

View full text Add to dashboard Cite

We report on IRAM-30m/EMIR observations of 38 Herschel sources chosen as the brightest red sub-millimeter (sub-mm) sources in 18 Planck-selected fields drawn from the Planck high-z (PHz) protocluster candidates sample. These fields host overdensities of red Herschel sources, with high star formation rates (∼10,000 M yr −1 ) as derived from Planck measurements. The goals of these observations are to measure spectroscopic redshifts of the Herschel sources in the PHz fields, investigate the origin of their bright sub-mm emission, and find evidence of their association with high-z protoclusters. We detect 40 CO lines on a total of 24 bright (S 350µm >40 mJy) Herschel sources in 14 of the 18 PHz fields. The measured average redshift is = 2.25±0.09, spanning a range from 1.32 to 2.75. We measure redshifts for multiple Herschel sources in close projected proximity in eight PHz fields. In half of those fields we detect from two to three objects at similar redshifts, supporting the idea that the PHz fields contain high-z protoclusters. The detection of sources at different redshifts in the same field demonstrates that foreground and background sources also contribute to the total sub-mm emission. We compare the properties of the molecular gas, and of the star formation activity of our sources with samples of normal star-forming galaxies (SFGs), sub-mm galaxies (SMGs), and CO-detected cluster and protocluster galaxies drawn from the literature at similar redshifts. We find that the PHz-IRAM sources are mainly normal SFGs, with only ∼20% undergoing a starburst phase. The PHz-IRAM sources are characterized by star formation rates ( = 1043±157 M yr −1 ) and gas masses ( = (4.0±0.7)×10 11 M ) that are, on average, eight and five times higher than those typical of normal SFGs at similar redshifts. Their dust temperatures ( = 29.2±0.9 K), and depletion timescales (<τ dep >=0.47±0.07 Gyr) are instead consistent with those of normal SFGs. The analysis of the CO spectral line energy distribution, available for ten PHz-IRAM sources, peaks at a low quantum rotation number (J up = 3) in most of the cases, implying low gas excitation. These properties imply that a significant fraction of the PHz-IRAM sources contains extended, and cold molecular gas reservoirs at low excitation, and that their star-formation is driven by secular processes. Multiplicity and moderate gravitational lensing might also play a role in producing the observed properties. Some of these properties are also observed in other CO-detected infrared-luminous protocluster galaxies at z 1.3-3. We find that the highest star-forming protoclusters drawn from the largest volume simulations available to date, have similar SFRs as the PHz protoclusters, but separate out into a larger number of star-forming galaxies. Millimeter and CO observations at higher spatial resolution than those presented here would be necessary to further elucidate the properties of our PHz-IRAM sources, and determine which mechanisms drive star-formation in infrared-lum...

show abstract

Section: The Molecular Gas Properties Of the Phz-iram Sourcesmentioning

confidence: 90%

Molecular gas properties of Planck-selected protocluster candidates at z~1.3-3

Polletta,

Dole,

Martinache

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…An alternative (albeit unlikely) explanation for the observed properties might be the presence of molecular gas on large-scale in the circumgalactic medium, as observed in some other protoclusters (Emonts et al 2016;Ginolfi et al 2017) and also in isolated quasars (see Cicone et al 2021). It is also possible that these massive, extended, and poorly excited molecular gas reservoirs are due to the combined emission of multiple galaxies at similar redshifts (with the low excitation caused by the decreasing beam size in EMIR at increasing frequencies).…”

Section: Molecular Gas Properties Of the Phz-iram Sourcesmentioning

confidence: 97%

Molecular gas properties of Planck-selected protocluster candidates at z ≃ 1.3–3

Polletta

Dole

Martinache

et al. 2022

A&A

View full text Add to dashboard Cite

We report on IRAM 30-m/EMIR observations of 38 Herschel sources chosen as the brightest red submillimeter (submm) sources in 18 Planck-selected fields drawn from the Planck high-z (PHz) sample of protocluster candidates. These fields host overdensities of red Herschel sources, with high star formation rates (∼10 000 M⊙ yr−1), as obtained from the Planck measurements. The goals of these observations are to measure the spectroscopic redshifts of the Herschel sources in the PHz fields, investigate the origin of their bright submm emission, and find evidence of their association with high-z protoclusters. We detected 40 CO lines on a total of 24 bright (S350 μm > 40 mJy) Herschel sources in 14 of the 18 PHz fields. The measured average redshift is ⟨zCO⟩ = 2.25 ± 0.09, spanning a range from 1.32 to 2.75. We measured the redshifts for multiple Herschel sources in projected proximity in eight PHz fields. In half of those fields, we detected between two and three objects at similar redshifts, supporting the idea that the PHz fields contain high-z protoclusters. The detection of sources at different redshifts in the same field demonstrates that foreground and background sources also contribute to the total submm emission. We compared the properties of the molecular gas and of the star formation activity of our sources with samples of normal star-forming galaxies (SFGs), submm galaxies (SMGs), and CO-detected cluster and protocluster galaxies drawn from the literature at similar redshifts. We find that the PHz-IRAM sources are mainly normal SFGs, with only ∼20% undergoing a starburst phase. The PHz-IRAM sources are characterized by star formation rates (⟨SFR⟩ = 1043 ± 157 M⊙ yr−1) and gas masses (⟨Mgas⟩ = (4.0 ± 0.7) × 1011 M⊙) that are, on average, eight and five times higher than those typical of normal SFGs at similar redshifts. Their dust temperatures (⟨Tdust⟩ = 29.2 ± 0.9 K) and depletion timescales (⟨τdep⟩ = 0.47 ± 0.07 Gyr) are instead consistent with those of normal SFGs. The analysis of the CO spectral line energy distribution, available for ten PHz-IRAM sources, peaks at a low quantum rotation number (Jup = 3) in most of the cases, implying low gas excitation. These properties imply that a significant number of PHz-IRAM sources contain extended and cold molecular gas reservoirs at low excitation and that their star formation is driven by secular processes. Multiplicity and moderate gravitational lensing might also play a role in producing the observed properties. Some of these properties are also observed in other CO-detected infrared-luminous protocluster galaxies at z ≃ 1.3 − 3. We find that the protoclusters with the highest level of star formation, drawn from the largest volume simulations available to date, exhibit similar SFRs as compared to the PHz protoclusters; however, they separate out into a higher number of star-forming galaxies. Millimeter and CO observations at higher spatial resolution than those presented here would be necessary to further elucidate the properties of our PHz-IRAM sources and determine which mechanisms drive star formation in infrared-luminous protocluster galaxies.

show abstract

“…ACA observations of one of the SUPER galaxies in CO(3-2) emission revealed evidence for a large amount of molecular gas out to 𝑟 ∼ 200 kpc (CID_346; Cicone et al 2021), implying an enormous history of outflows that enriched the CGM out to large radii. Unfortunately a deeper ACA CO(3-2) observation of this source does not reveal evidence for any significant emission beyond 𝑟 ∼ 10 kpc (Jones et al submitted).…”

Section: Comparison To Other Detections Of Extended Gas Emissionmentioning

confidence: 99%

Evidence for extended gaseous reservoirs around AGN at cosmic noon from ALMA CO(3−2) observations

Jones

Maiolino

Circosta

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Gaseous outflows are key phenomena in the evolution of galaxies, as they affect star formation (either positively or negatively), eject gas from the core or disk, and directly cause mixing of pristine and processed material. Active outflows may be detected through searches for broad spectral line emission or high-velocity gas, but it is also possible to determine the presence of past outflows by searching for extended reservoirs of chemically enriched molecular gas in the circumgalactic medium (CGM) around galaxies. In this work, we examine the CO(3-2) emission of a set of seven z ∼ 2.0 − 2.5 AGN host galaxies, as observed with ALMA. Through a three-dimensional stacking analysis we find evidence for extended CO emission of radius r ∼ 13 kpc. We extend this analysis to the HST/ACS i-band images of the sample galaxies, finding a complex small-scale (r < 10 kpc) morphology but no robust evidence for extended emission. In addition, the dust emission (traced by rest-frame FIR emission) shows no evidence for significant spatial extension. This indicates that the diffuse CO emission revealed by ALMA is morphologically distinct from the stellar component, and thus traces an extended reservoir of enriched gas. The presence of a diffuse, enriched molecular reservoir around this sample of AGN host galaxies at cosmic noon hints at a history of AGN-driven outflows that likely had strong effects on the star formation history of these objects.

show abstract

Super

Cited by 24 publications

References 34 publications

Molecular gas properties of Planck-selected protocluster candidates at z~1.3-3

Molecular gas properties of Planck-selected protocluster candidates at z~1.3-3

Molecular gas properties of Planck-selected protocluster candidates at z ≃ 1.3–3

Evidence for extended gaseous reservoirs around AGN at cosmic noon from ALMA CO(3−2) observations

Contact Info

Product

Resources

About