Gas and dust cooling along the major axis of M 33 (HerM33es)

Krämer, C.; Nikola, Thomas; Anderl, S.; Bertoldi, F.; Boquien, M.; Braine, J.; Buchbender, C.; Combes, F.; Henkel, C.; Hermelo, I.; Israel, F. P.; Relaño, M.; Röllig, M.; Schuster, K.; Tabatabaei, F. S.; Tak, F. F. S. van der; Verley, S.; Werf, P. van der; Wiedner, Martina C.; Xilouris, E. M.

doi:10.1051/0004-6361/201936754

Cited by 12 publications

(6 citation statements)

References 68 publications

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“…More recently, Kramer et al (2020) reported an 𝑅 CII OI63 = 0.2 − 20 in M33 with a mean of 4.5 ± 2.6 which matches with the Kaufman et al (2006) one-dimensional uniform density PDR models of 𝑛 H ∼ 2 × 10 2 − 10 4 cm −3 interacting with 𝐺 0 ∼ 1.5 − 60. After experimenting with such simple PDR models, we also confirm the observed ratio of Kramer et al (2020) using 3 -in one-dimensional slabs but we are unable to reproduce this ratio with our full three-dimensional models. We therefore conclude that a ratio between these two lines is rather challenging to use as a diagnostic (see also Kraemer et al 1998).…”

Section: Line Ratiossupporting

confidence: 62%

Photodissociation Region Diagnostics Across Galactic Environments

Bisbas,

Tan,

Tanaka

2020

Preprint

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We present three-dimensional astrochemical simulations and synthetic observations of magnetised, turbulent, self-gravitating molecular clouds. We explore various galactic interstellar medium environments, including cosmic-ray ionization rates in the range of 𝜁 CR = 10 −17 -10 −14 s −1 , far-UV intensities in the range of 𝐺 0 = 1-10 3 and metallicities in the range of 𝑍 = 0.1-2 Z . The simulations also probe a range of densities and levels of turbulence, including cases where the gas has undergone recent compression due to cloud-cloud collisions. We examine: i) the column densities of carbon species across the cycle of C , C and CO, along with O , in relation to the H -to-H 2 transition; ii) the velocity-integrated emission of [C ] 158𝜇m, [ 13 C ] 158𝜇m, [C ] 609𝜇m and 370𝜇m, [O ] 63𝜇m and 146𝜇m, and of the first ten 12 CO rotational transitions; iii) the corresponding Spectral Line Energy Distributions; iv) the usage of [C ] and [O ] 63𝜇m to describe the dynamical state of the clouds; v) the behavior of the most commonly used ratios between transitions of CO and [C ]; and vi) the conversion factors for using CO and C as H 2 -gas tracers. We find that enhanced cosmic-ray energy densities enhance all aforementioned line intensities. At low metallicities, the emission of [C ] is well connected with the H 2 column, making it a promising new H 2 tracer in metal-poor environments. The conversion factors of 𝑋 CO and 𝑋 CI depend on metallicity and the cosmic-ray ionization rate, but not on FUV intensity. In the era of ALMA, SOFIA and the forthcoming CCAT-prime telescope, our results can be used to understand better the behaviour of systems in a wide range of galactic and extragalactic environments.

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Section: Line Ratiossupporting

confidence: 62%

Photodissociation Region Diagnostics Across Galactic Environments

Bisbas,

Tan,

Tanaka

2020

Preprint

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“…This is sufficient to associate most of the [C II] emission with a PDR, start probing the physical conditions around a single H II region, and suggest the presence of CO-dark molecular gas (Braine et al 2012). Based on the comparison of [C II], [O I] and TIR emission with PDR models, Kramer et al (2020) infer a relatively homogeneous medium on these scales in M33, with the large-scale average gas properties being similar to the average of the gas properties measured in four individual regions; namely: a moderate density (n∼2 × 10 2 cm −3 ) and radiation field (G0∼60), with a relatively low beam filling factor of the PDRs, defined as the ratio between the radiation field constrained from the modeling and the radiation field inferred from the observed TIR emission (f b ∼1 by contrast to a larger value enabled by the presence of several PDRs on the line of sight). No difference was detected between the inner and outer parts of the galaxy.…”

Section: Mapping and Velocity Resolved Observations Applied To Galaxiesmentioning

confidence: 99%

Photodissociation and X-Ray Dominated Regions

Wolfire¹,

Vallini²,

Chevance³

2022

Preprint

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The radiation from stars and active galactic nuclei (AGN) creates photodissociation regions (PDRs) and X-ray dominated regions (XDRs), where the chemistry or heating are dominated by far-ultraviolet (FUV) radiation or X-ray radiation, respectively. PDRs include a wide range of environments from the diffuse interstellar medium to dense star-forming regions. XDRs are found in the center of galaxies hosting AGN, in protostellar disks, and in the vicinity of X-ray binaries. In this review, we describe the dominant thermal, chemical, and radiation transfer processes in PDRs and XDRs, as well as a brief description of models and their use to analyze observations. We then present recent results from Milky Way, nearby extragalactic, and high-redshift observations. Several important results are:

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“…It is also easily self-absorbed; small amounts of cold foreground gas can absorb [OI]63µm while leaving [OI]146µm unaffected (Liseau et al 2006). This effect has been measured to reduce the [OI]63µm emission by factors of 1.3 ± 1.8 (Kramer et al 2020) up to 2.9 ± 1.6 (Liseau et al 2006). If [OI]63µm/[OI]146µm < 10, [OI]63µm is likely self-absorbed (Díaz-Santos et al 2017;Cormier et al 2015;Tielens & Hollenbach 1985).…”

Section: Also Found Lower [Oi]63µmmentioning

confidence: 99%

Multi-Phase ISM in the z = 5.7 Hyperluminous Starburst SPT0346-52

Litke,

Marrone,

Aravena

et al. 2022

Preprint

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SPT0346-52 (z = 5.7) is the most intensely star-forming galaxy discovered by the South Pole Telescope, with Σ SFR ∼ 4200 M yr −1 kpc −2 . In this paper, we expand on previous spatially-resolved studies, using ALMA observations of dust continuum, [NII]205µm, [CII]158µm, [OI]146µm, and undetected [NII]122µm and [OI]63µm emission to study the multi-phase interstellar medium (ISM) in SPT0346-52. We use pixelated, visibility-based lens modeling to reconstruct the source-plane emission. We also model the source-plane emission using the photoionization code cloudy and find a supersolar metallicity system. We calculate T dust = 48.3 K and λ peak = 80µm, and see line deficits in all five lines. The ionized gas is less dense than comparable galaxies, with n e < 32 cm −3 , while ∼ 20% of the [CII]158 emission originates from the ionized phase of the ISM. We also calculate the masses of several phases of the ISM. We find that molecular gas dominates the mass of the ISM in SPT0346-52, with the molecular gas mass ∼ 4× higher than the neutral atomic gas mass and ∼ 100× higher than the ionized gas mass.

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Gas and dust cooling along the major axis of M 33 (HerM33es)

Cited by 12 publications

References 68 publications

Photodissociation Region Diagnostics Across Galactic Environments

Photodissociation Region Diagnostics Across Galactic Environments

Photodissociation and X-Ray Dominated Regions

Multi-Phase ISM in the z = 5.7 Hyperluminous Starburst SPT0346-52

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