A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies

Díaz-Santos, T.; Armus, L.; Charmandaris, V.; Lu, N.; Stierwalt, Sabrina; Stacey, G. J.; Malhotra, Sangeeta; Werf, P. P. van der; Howell, Justin; Privon, George C.; Mazzarella, J. M.; Goldsmith, Paul F.; Murphy, E. J.; Barcos-Muñoz, Loreto; Linden, Sean T.; Inami, Hanae; Larson, Kirsten L.; Evans, A. S.; Appleton, P. N.; Iwasawa, K.; Lord, S. D.; Sanders, D. B.; Surace, J.

doi:10.3847/1538-4357/aa81d7

Cited by 243 publications

(360 citation statements)

References 130 publications

(222 reference statements)

Supporting

Mentioning

311

Contrasting

Unclassified

Order By: Relevance

“…The authors suggest that the [C II] deficit is driven by local physical processes of interstellar gas (e.g., [C II] self-absorption, dust extinction, and dust grain charge), not related to the global properties of the galaxies. Another study of spatially resolved local galaxies in the GOALS sample, by Díaz-Santos et al (2017), likewise suggest that local processes are the cause of the [C II] deficit; they propose that the radiation field strength to gas density ratio is the driver.…”

Section: By Exploring the [ ]mentioning

confidence: 99%

“…For galaxies with L FIR <10 11 L e , the [ ] L C II /L FIR ratio is constant at ∼1%; however, at L FIR >10 11 L e , the [ ] L C II /L FIR ratio decreases to ∼0.1%-0.01%. This decrease is known as the "[C II] deficit," and many attempts have been made over the past two decades to investigate its origin (e.g., Hailey-Dunsheath et al 2010;Ivison et al 2010;Stacey et al 2010;Graciá-Carpio et al 2011;Valtchanov et al 2011;Farrah et al 2013;Gullberg et al 2015;Lutz et al 2016;Díaz-Santos et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…This follows the relation seen by Smith et al (2017) for local star-forming galaxies. A higher star formation rate surface density in the L C II to L FIR ratio as a function of the star formation rate density for local galaxies in the KINGFISH and GOALS (Armus et al 2009;Lutz et al 2016;Díaz-Santos et al 2017), a sample of high-redshift galaxies (Wang et al 2013;Capak et al 2015;Gullberg et al 2015;Kimball et al 2015;Lutz et al 2016;Nesvadba et al 2016;Díaz-Santos et al 2017;Jones et al 2017;Umehata et al 2017;Venemans et al 2017), and our sample of four z∼4.5 SMGs. We note that the sizes used to achieve the star formation rate densities for the GOALS sample are the 70 μm effective radii under the assumption of a uniform dust temperature.…”

mentioning

confidence: 99%

“…In particular, they emphasize the importance of a varying radiation field strength to gas density ratio (G n gas ). Díaz-Santos et al (2017) fit a power law to local ULIRGs from GOALS (see Equation (3) in Díaz-Santos et al 2017) and find that the suppression of the [C II] to far-infrared luminosity ratio at high far-infrared surface densities could be due to high G n gas ratios. Using semi-analytical models, Lagache et al (2018) likewise suggest that the [C II] to farinfrared deficit is correlated with the intensity of the interstellar radiation field.…”

mentioning

confidence: 99%

“…The inner parts of our four galaxies are plotted as red circles and the outer annuli as stars. , and the curved power law fitted to galaxies in GOALS from (Díaz-Santos et al 2017) is plotted as the dotted-dashed curve. We note that both the high-and low-redshift samples exhibit a large scatter around the two models.…”

mentioning

confidence: 99%

See 4 more Smart Citations

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

Gullberg

Swinbank

Smail

et al. 2018

ApJ

View full text Add to dashboard Cite

Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C II] λ157.7 μm emission in four z∼4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 μm (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations (s~-27 47 345 GHz μJy beam −1 ). The four SMGs are bright [C II] emitters. We extract [C II] spectra from the high-resolution data, and recover ∼20%-100% of the [C II] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C II] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 μm dust continuum by a factor of 1.6±0.4. By considering the [ ] L C II /L FIR ratio as a function of the star formation rate surface density (S SFR ), we revisit the [C II] deficit and suggest that the decline in the [ ] L C II /L FIR ratio as a function of S SFR is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.

show abstract

Section: By Exploring the [ ]mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

See 3 more Smart Citations

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

Gullberg

Swinbank

Smail

et al. 2018

ApJ

View full text Add to dashboard Cite

show abstract

Starbursts versus active galactic nuclei: Studying astrochemistry of dusty galaxies

Martins-Franco

Menéndez‐Delmestre

2021

Astron Nachr

View full text Add to dashboard Cite

Infrared luminous galaxies are rare locally but dominate the star formation activity at z ≥ 1. The study of these objects is difficult at optical wavelengths especially on account of the abundant dust. At the smallest scales, dust becomes micron-sized molecules known as PAHs that are excited by UV photons and whose emission can be used to reveal physical properties of obscured regions that otherwise remain invisible to our instruments. We can thus use infrared spectroscopy to classify the emission in these systems as arising from star formation activity or active galactic nuclei (AGN). In this work, we go further than this and undertake an astrochemical analysis of the ISM by probing the PAH population. Based on Spitzer/IRS mid-infrared spectra of ∼700 dusty galaxies from the GOALS and ATLAS surveys, we analyze the PAH population in terms of size, charge, and composition using the NASA Ames PAH Database, a large theoretical spectroscopic library of PAH molecules. We find that the PAH population in these galaxies is dominated by small and neutral molecules, with very little diversity in composition, beyond Carbon and Hydrogen. These results are consistent with theoretical models of PAH emission for star-forming galaxies. We also see a weak trend of an increased proportion of charged PAHs in galaxies with a more pronounced AGN contribution, suggesting that the radiation field of the power source may ultimately affect the ISM astrochemistry. Although our results point to AGN being capable of altering PAHs molecules, PAH features are still significant in AGN regions, suggesting that the AGN does not destroy them. This is in agreement with recent laboratory works pointing and motivating further use of PAH molecules to probe for the radiation field in these dusty, extreme environments.

show abstract

Star formation and nuclear activity in luminous infrared galaxies: an infrared through radio review

Pérez-Torres

Mattila

Alonso‐Herrero

et al. 2021

Astron Astrophys Rev

View full text Add to dashboard Cite

A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies

Cited by 243 publications

References 130 publications

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

Starbursts versus active galactic nuclei: Studying astrochemistry of dusty galaxies

Star formation and nuclear activity in luminous infrared galaxies: an infrared through radio review

Contact Info

Product

Resources

About