Photodissociation and X-Ray Dominated Regions

Wolfire, M. G.; Vallini, L.; Chevance, Mélanie

doi:10.48550/arxiv.2202.05867

Cited by 13 publications

(24 citation statements)

References 409 publications

(719 reference statements)

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“…This value is at the lower end of the distribution found for QSOs at this redshift (Walter et al 2022;Decarli et al 2018;Shao et al 2019). The neutral gas mass in the disk, based on [CII] emission, can be derived with the relation from Hailey-Dunsheath et al (2010) (see also Bischetti et al 2019b), where X C + is the [CII] fraction per hydrogen atom, T is the gas temperature, n is the gas density, and n crit ∼ 3 × 10 3 cm −3 is the [CII]λ158µm critical density for collisions with neutral hydrogen that frequently occur in photo-dissociation regions (PDRs; Wolfire et al 2022;Hollenbach & Tielens 1999). We estimated the lower limit for the molecular mass in the regime n n crit (Maiolino et al 2005;Aalto et al 2012Aalto et al , 2015, and we considered a X C + ∼ 10 −4 and a gas temperature of 200 K, both typical of PDRs (Maiolino et al 2005;Hailey-Dunsheath et al 2010;Cicone et al 2015;Bischetti et al 2019a).…”

Section: [Cii] Distribution and Kinematicsmentioning

confidence: 99%

Black hole and host galaxy growth in an isolated z ∼ 6 QSO observed with ALMA

Tripodi

Feruglio

Fiore

et al. 2022

A&A

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The outstanding mass growth of supermassive black holes (SMBHs) at the epoch of reionisation and its relation to the concurrent growth of their host galaxies poses challenges to theoretical models aimed at explaining how these systems formed on short timescales (<1 Gyr). To trace the average evolutionary paths of quasi-stellar objects (QSOs) and their host galaxies in the plane of BH mass to host mass (M dyn ), we compare the star formation rate (SFR), derived from the accurate estimate of the dust temperature and the dust mass (T dust , M dust ) based on infrared and sub-millimeter (sub-mm) spectral energy distribution (SED), with the BH accretion rate, derived from L bol based on X-ray and optical and ultraviolet SED. To this aim, we analysed a deep ALMA observation of the submm continuum, [CII], and H 2 O of the z ∼ 6 QSO J2310+1855 with a resolution of 900 pc, which enabled a detailed study of dust properties and cold gas kinematics. We performed an accurate SED analysis obtaining a dust temperature of T dust = 71 ± 4 K, dust mass M dust = (4.4 ± 0.7) × 10 8 M , and total far-infrared luminosity of L TIR = 2.5 +0.6 −0.5 × 10 13 L . The implied active galactic nuclei (AGN) -corrected SFR = 1240 +310 −260 M yr −1 is a factor of 2 lower than previously reported for this QSO. We measured a gas-to-dust ratio of GDR= 101 ± 20. The dust continuum and [CII] surface brightness profiles are spatially extended out to r ∼ 6.7 kpc and r ∼ 5 kpc, respectively, with half-light radii of 0.9 and 1.1 kpc for the dust and gas, respectively. The derived gas surface density, Σ gas , and star formation rate density, Σ SFR , place the J2310+1855 host galaxy above the Kennicutt-Schmidt relation. We derived a best estimate of the dynamical mass M dyn = 5.2 × 10 10 M within r = 1.7 kpc based on a dynamical model of the system with a rotating disk inclined at i = 25 deg. The Toomre parameter profile across the disk is Q gas ∼ 3 and implies that the disk is unstable. We found that SFR/M dyn > ṀBH /M BH , suggesting that AGN feedback might be efficiently acting to slow down the SMBH accretion, while stellar mass assembly is still vigorously taking place in the host galaxy. In addition, we were also able to detect high-velocity emission on the red and blue sides of the [CII] emission line that is not consistent with disk rotation and traces a gaseous outflow. We derived an outflow mass M out = 3.5 × 10 8 M , and a mass outflow rate in the range Ṁout = 1800 − 4500 M yr −1 . The implied Ėout ∼ 0.0005−0.001 L bol is in agreement with the values observed for ionised winds. For the first time, we mapped a spatially resolved water vapour disk through the H 2 O v=0 3 (2,2) − 3 (1,3) emission line detected at ν obs = 274.074 GHz, whose kinematic properties and size are broadly consistent with those of the [CII] disk. The luminosity ratio L H 2 O /L TIR = 1.4 × 10 −5 is consistent with line excitation by dust-reprocessed star formation in the interstellar medium of the host galaxy.

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Section: [Cii] Distribution and Kinematicsmentioning

confidence: 99%

Black hole and host galaxy growth in an isolated z ∼ 6 QSO observed with ALMA

Tripodi

Feruglio

Fiore

et al. 2022

A&A

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“…Intensity mapping experiments aim to detect the large-scale collective line emission from galaxies using widefield spectral mapping. The [CII] line at 158 µm is one of the main cooling lines of the interstellar medium (e.g., Tielens & Hollenbach 1985;Wolfire et al 2022). Observational studies at low redshift (e.g., De Looze et al 2014;Herrera-Camus et al 2015) and high redshift (e.g., Capak et al 2015;Schaerer et al 2020;Carniani et al 2020) found a non-evolving and nearlylinear empirical correlation between [CII] luminosity and SFR.…”

Section: Introductionmentioning

confidence: 99%

CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping

Bethermin,

Gkogkou,

Van Cuyck

et al. 2022

Preprint

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The intensity mapping of the [CII] 158 µm line redshifted to the submillimeter window is a promising probe of the z>4 star formation and its spatial distribution into the large-scale structure. To prepare the first-generation experiments (e.g., CONCERTO), we need realistic simulations of the submillimeter extragalactic sky in spectroscopy. We present a new version of the simulated infrared dusty extragalactic sky (SIDES) including the main submillimeter lines around 1 mm (CO, [CII], [CI]). This approach successfully reproduces the observed line luminosity functions. We then use our simulation to generate CONCERTO-like cubes (125-305 GHz) and forecast the power spectra of the fluctuations caused by the various astrophysical components at those frequencies. Depending on our assumptions on the relation between star formation rate and [CII] luminosity, and the star formation history, our predictions of the z∼6 [CII] power spectrum vary by two orders of magnitude. This highlights how uncertain the predictions are and how important future measurements will be to improve our understanding of this early epoch. SIDES can reproduce the CO shot noise recently measured at ∼100 GHz by the mmIME experiment. Finally, we compare the contribution of the different astrophysical components at various redshift to the power spectra. The continuum is by far the brightest, by a factor of 3 to 100 depending on the frequency. At 300 GHz, the CO foreground power spectrum is higher than the [CII] one for our base scenario. At lower frequency, the contrast between [CII] and extragalactic foregrounds is even worse. Masking the known galaxies from deep surveys should allow to reduce the foregrounds to 20 % of the [CII] power spectrum up to z∼6.5. However, this masking method will not be sufficient at higher redshifts. The code and the products of our simulation are released publicly and can be used for both intensity mapping experiments and submillimeter continuum and line surveys.

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“…In their most general definitionneutral gas regulated by FUV radiation -, PDRs represent the dominant fraction of the neutral atomic and molecular gas in the ISM of starforming galaxies [1,3]. Indeed, except for the cold and dense molecular cores associated with the first stages of star formation, most of the ISM (in volume and mass) is effectively at A V < 8 mag.…”

Section: Pdrs Everywherementioning

confidence: 99%

Multi-line Observations, Models, and Data Needed to Understand the Nature of UV-irradiated Interstellar Matter

Goicoechea¹,

Cuadrado²,

Petit³

2022

Preprint

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Far-ultraviolet photons from OB-type massive stars regulate the heating, ionization, and chemistry of much of the neutral interstellar gas in starforming galaxies. The interaction of FUV radiation and interstellar matter takes place in environments broadly known as photodissociation regions (PDRs). PDR line diagnostics are the smoking gun of the radiative feedback from massive stars. Improving our understanding of stellar feedback in the ISM requires quantifying the energy budget, gas dynamics, and chemical composition of PDR environments. This goal demands astronomical instrumentation able to deliver multi-line spectroscopic images of the ISM (of the Milky Way and nearby galaxies). It also requires interdisciplinary collaborations to obtain the rate coefficients and cross sections of the many microphysical processes that occur in the ISM and that are included in models such as the Meudon PDR code.

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Photodissociation and X-Ray Dominated Regions

Cited by 13 publications

References 409 publications

Black hole and host galaxy growth in an isolated z ∼ 6 QSO observed with ALMA

Black hole and host galaxy growth in an isolated z ∼ 6 QSO observed with ALMA

CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping

Multi-line Observations, Models, and Data Needed to Understand the Nature of UV-irradiated Interstellar Matter

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