Synthetic observations of star formation and the interstellar medium

Haworth, Thomas J.; Glover, Simon C. O.; Koepferl, Christine; Bisbas, Thomas G.; Dale, James E.

doi:10.1016/j.newar.2018.06.001

Cited by 39 publications

(33 citation statements)

References 624 publications

(834 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…They also find that, when comparing to H I intensity power spectra of nearby galaxies, the small-scale power spectra are dominated by the PSF shape. These results demonstrate the need to produce synthetic observations when comparing power spectra of simulations and observations (Haworth et al 2018). Our results provide a benchmark for comparing observations and simulations of Local Group-like galaxies.…”

Section: Discussionmentioning

confidence: 66%

“…Even if multiple spatial distributions yield the same power spectrum index, our results still a key benchmark for simulations that aim to reproduce Local Group-like galaxies. Several recent works aim to simulate galaxies with properties closely matching the LMC, SMC, M31, M33, or the Milky Way (Combes et al 2012;Wetzel et al 2016;Grisdale et al 2017;Dobbs et al 2018;Garrison-Kimmel et al 2019) with many producing "synthetic" observations to compare with properties found in the actual observations (e.g., Dobbs et al 2019), a key step for directly comparing simulations and observations (Haworth et al 2018). For any simulation the produces dust maps or synthetic IR observations, matching our measured power spectrum represents an important check.…”

Section: Variation In the Power Spectrum Index Between Galaxiesmentioning

confidence: 92%

See 1 more Smart Citation

Spatial power spectra of dust across the Local Group: No constraint on disc scale height

Koch

Chiang

Utomo

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We analyze the 1D spatial power spectra of dust surface density and mid to far-infrared emission at 24-500 µm in the LMC, SMC, M31, and M33. By forward-modelling the pointspread-function (PSF) on the power spectrum, we find that nearly all power spectra have a single power-law and point source component. A broken power-law model is only favoured for the LMC 24 µm MIPS power spectrum and is due to intense dust heating in 30 Doradus. We also test for local power spectrum variations by splitting the LMC and SMC maps into 820 pc boxes. We find significant variations in the power-law index with no strong evidence for breaks. The lack of a ubiquitous break suggests that the spatial power spectrum does not constrain the disc scale height. This contradicts claims of a break where the turbulent motion changes from 3D to 2D. The power spectrum indices in the LMC, SMC, and M31 are similar (2.0-2.5). M33 has a flatter power spectrum (1.3), similar to more distant spiral galaxies with a centrally-concentrated H 2 distribution. We compare the power spectra of H I, CO, and dust in M31 and M33, and find that H I power spectra are consistently flatter than CO power spectra. These results cast doubt on the idea that the spatial power spectrum traces large scale turbulent motion in nearby galaxies. Instead, we find that the spatial power spectrum is influenced by (1) the PSF on scales below ∼ 3 times the FWHM, (2) bright compact regions (30 Doradus), and (3) the global morphology of the tracer (an exponential CO disc).

show abstract

Section: Discussionmentioning

confidence: 66%

Section: Variation In the Power Spectrum Index Between Galaxiesmentioning

confidence: 92%

Spatial power spectra of dust across the Local Group: No constraint on disc scale height

Koch

Chiang

Utomo

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…By post-processing such simulations to generate synthetic observations of (molecular) gas or SFR tracers (see e.g. Pawlik & Schaye 2011;da Silva et al 2012;Krumholz 2014;Haworth et al 2017), it is possible to derive the tracer lifetimes and test how the method's performance is affected by environmental variations in tracer emissivity. First efforts in this direction are currently in progress.…”

Section: Applicability and Future Workmentioning

confidence: 99%

An uncertainty principle for star formation – II. A new method for characterizing the cloud-scale physics of star formation and feedback across cosmic history

Kruijssen

Schruba

Hygate

et al. 2018

Monthly Notices of the Royal Astronomical Society

106

319

View full text Add to dashboard Cite

show abstract

“…In dynamical pictures of converging gas flows, cloud-cloud collisions and cloud collapse flows, a convergence of gas flows toward some point in space is involved. There is a major difference between converging gas flows and cloud-cloud collisions on the one hand and cloud collapse on the other: in the converging gas flow and cloud-cloud collision picture the compression is produced by some external cause (e.g., supernovae or spiral arm potentials, e.g., Mac Low & Klessen 2004;Haworth et al 2018;Kobayashi et al 2018), whereas the collapsing cloud flows are dominated by the self-gravity of the cloud itself (e.g., Vázquez-Semadeni et al 2019). In reality, externally driven converging flows may produce the clouds that then further collapse under their own self-gravity.…”

Section: Introductionmentioning

confidence: 99%

Dynamical cloud formation traced by atomic and molecular gas

Beuther

Wang

Soler

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Atomic and molecular cloud formation is a dynamical process. However, kinematic signatures of these processes are still observationally poorly constrained. Aims. We identify and characterize the cloud formation signatures in atomic and molecular gas. Methods. Targeting the cloud-scale environment of the prototypical infrared dark cloud G28.3, we employed spectral line imaging observations of the two atomic lines HI and [CI] as well as molecular lines observations in 13CO in the 1–0 and 3–2 transitions. The analysis comprises investigations of the kinematic properties of the different tracers, estimates of the mass flow rates, velocity structure functions, a histogram of oriented gradients (HOG) study, and comparisons to simulations. Results. The central infrared dark cloud (IRDC) is embedded in a more diffuse envelope of cold neutral medium traced by HI self-absorption and molecular gas. The spectral line data as well as the HOG and structure function analysis indicate a possible kinematic decoupling of the HI from the other gas compounds. Spectral analysis and position–velocity diagrams reveal two velocity components that converge at the position of the IRDC. Estimated mass flow rates appear rather constant from the cloud edge toward the center. The velocity structure function analysis is consistent with gas flows being dominated by the formation of hierarchical structures. Conclusions. The observations and analysis are consistent with a picture where the IRDC G28.3 is formed at the center of two converging gas flows. While the approximately constant mass flow rates are consistent with a self-similar, gravitationally driven collapse of the cloud, external compression (e.g., via spiral arm shocks or supernova explosions) cannot be excluded yet. Future investigations should aim at differentiating the origin of such converging gas flows.

show abstract

Synthetic observations of star formation and the interstellar medium

Cited by 39 publications

References 624 publications

Spatial power spectra of dust across the Local Group: No constraint on disc scale height

Spatial power spectra of dust across the Local Group: No constraint on disc scale height

An uncertainty principle for star formation – II. A new method for characterizing the cloud-scale physics of star formation and feedback across cosmic history

Dynamical cloud formation traced by atomic and molecular gas

Contact Info

Product

Resources

About