Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator

Jessica Sutter; Daniel A. Dale; Kevin V. Croxall; Eric W. Pelligrini; J. D.T. Smith; Philip N. Appleton; Pedro Beirão; Alberto D. Bolatto; Daniela Calzetti; Alison Crocker; Ilse De Looze; Bruce Draine; Maud Galametz; Brent A. Groves; George Helou; Rodrigo Herrera-Camus; Leslie K. Hunt; Robert C. Kennicutt; Hélène Roussel; Mark G. Wolfire

doi:10.3847/1538-4357/ab4da5

Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator

Jessica Sutter, Daniel A. Dale, Kevin V. Croxall, Eric W. Pelligrini, J. D.T. Smith, Philip N. Appleton, Pedro Beirão, Alberto D. Bolatto, Daniela Calzetti, Alison Crocker, Ilse De Looze, Bruce Draine, Maud Galametz, Brent A. Groves, George Helou, Rodrigo Herrera-Camus, Leslie K. Hunt, Robert C. Kennicutt, Hélène Roussel, Mark G. Wolfire

Astrophysical Sciences

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Abstract

The brightest observed emission line in many star-forming galaxies is the [C II} 158 μm line, making it detectable up to z ∼ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 158 μm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 μm and [N II] 205 μm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: A Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II]in the neutral and ionized phases of the ISM. We find that the[C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.

Original language	English (US)
Article number	60
Journal	Astrophysical Journal
Volume	886
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ab4da5
State	Published - Nov 20 2019

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ab4da5

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Sutter, J., Dale, D. A., Croxall, K. V., Pelligrini, E. W., Smith, J. D. T., Appleton, P. N., Beirão, P., Bolatto, A. D., Calzetti, D., Crocker, A., De Looze, I., Draine, B., Galametz, M., Groves, B. A., Helou, G., Herrera-Camus, R., Hunt, L. K., Kennicutt, R. C., Roussel, H., & Wolfire, M. G. (2019). Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator. Astrophysical Journal, 886(1), Article 60. https://doi.org/10.3847/1538-4357/ab4da5

@article{a403fb02cb974eb2916588d3e24f9080,

title = "Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator",

abstract = "The brightest observed emission line in many star-forming galaxies is the [C II} 158 μm line, making it detectable up to z ∼ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 158 μm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 μm and [N II] 205 μm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: A Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II]in the neutral and ionized phases of the ISM. We find that the[C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.",

author = "Jessica Sutter and Dale, {Daniel A.} and Croxall, {Kevin V.} and Pelligrini, {Eric W.} and Smith, {J. D.T.} and Appleton, {Philip N.} and Pedro Beir{\~a}o and Bolatto, {Alberto D.} and Daniela Calzetti and Alison Crocker and {De Looze}, Ilse and Bruce Draine and Maud Galametz and Groves, {Brent A.} and George Helou and Rodrigo Herrera-Camus and Hunt, {Leslie K.} and Kennicutt, {Robert C.} and H{\'e}l{\`e}ne Roussel and Wolfire, {Mark G.}",

year = "2019",

month = nov,

day = "20",

doi = "10.3847/1538-4357/ab4da5",

language = "English (US)",

volume = "886",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

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Sutter, J, Dale, DA, Croxall, KV, Pelligrini, EW, Smith, JDT, Appleton, PN, Beirão, P, Bolatto, AD, Calzetti, D, Crocker, A, De Looze, I, Draine, B, Galametz, M, Groves, BA, Helou, G, Herrera-Camus, R, Hunt, LK, Kennicutt, RC, Roussel, H & Wolfire, MG 2019, 'Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator', Astrophysical Journal, vol. 886, no. 1, 60. https://doi.org/10.3847/1538-4357/ab4da5

TY - JOUR

T1 - Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator

AU - Sutter, Jessica

AU - Dale, Daniel A.

AU - Croxall, Kevin V.

AU - Pelligrini, Eric W.

AU - Smith, J. D.T.

AU - Appleton, Philip N.

AU - Beirão, Pedro

AU - Bolatto, Alberto D.

AU - Calzetti, Daniela

AU - Crocker, Alison

AU - De Looze, Ilse

AU - Draine, Bruce

AU - Galametz, Maud

AU - Groves, Brent A.

AU - Helou, George

AU - Herrera-Camus, Rodrigo

AU - Hunt, Leslie K.

AU - Kennicutt, Robert C.

AU - Roussel, Hélène

AU - Wolfire, Mark G.

PY - 2019/11/20

Y1 - 2019/11/20

N2 - The brightest observed emission line in many star-forming galaxies is the [C II} 158 μm line, making it detectable up to z ∼ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 158 μm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 μm and [N II] 205 μm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: A Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II]in the neutral and ionized phases of the ISM. We find that the[C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.

AB - The brightest observed emission line in many star-forming galaxies is the [C II} 158 μm line, making it detectable up to z ∼ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 158 μm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 μm and [N II] 205 μm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: A Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II]in the neutral and ionized phases of the ISM. We find that the[C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.

UR - http://www.scopus.com/inward/record.url?scp=85077869614&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85077869614&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ab4da5

DO - 10.3847/1538-4357/ab4da5

M3 - Article

AN - SCOPUS:85077869614

SN - 0004-637X

VL - 886

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 60

ER -

Using [C II] 158 μm Emission from isolated ism phases as a star formation rate indicator

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