Submillimeter detection of extragalactic C I emission: IC 342

Thomas H. Büttgenbach; Jocelyn Keene; T. G. Phillips; Christopher K. Walker

Submillimeter detection of extragalactic C I emission: IC 342

Thomas H. Büttgenbach, Jocelyn Keene, T. G. Phillips, Christopher K. Walker

Research output: Contribution to journal › Article › peer-review

Abstract

We report observations of the ³P₁ → ³P₀ transition of atomic carbon at 492 GHz in IC 342, made at the Caltech Submillimeter Observatory, which represent the first extragalactic submillimeter detection of C I. The C I emission from IC 342 was found to have a main beam temperature of about 1 K, which is a factor of 2 greater than that for ¹³CO(2 → 1) in the same size beam. Comparing our data with COBE observations of the Milky Way, we find that the ratio of C I to CO(2 → 1) is approximately a factor of 2 lower in IC 342 than in our Galaxy. The result is interpreted in terms of photodissociation region models which require higher gas densities for IC 342 than for the Milky Way.

Original language	English (US)
Pages (from-to)	L15-L17
Journal	Astrophysical Journal
Volume	397
Issue number	1 PART 2
State	Published - Sep 20 1992

Keywords

Galaxies: individual: IC 342
Galaxies: interstellar matter
ISM: general
Infrared: interstellar: lines
Radio lines: atomic
Radio lines: molecular: interstellar

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Cite this

@article{50b3e3c4ab894c3fac3406e4782a8e52,

title = "Submillimeter detection of extragalactic C I emission: IC 342",

abstract = "We report observations of the 3P1 → 3P0 transition of atomic carbon at 492 GHz in IC 342, made at the Caltech Submillimeter Observatory, which represent the first extragalactic submillimeter detection of C I. The C I emission from IC 342 was found to have a main beam temperature of about 1 K, which is a factor of 2 greater than that for 13CO(2 → 1) in the same size beam. Comparing our data with COBE observations of the Milky Way, we find that the ratio of C I to CO(2 → 1) is approximately a factor of 2 lower in IC 342 than in our Galaxy. The result is interpreted in terms of photodissociation region models which require higher gas densities for IC 342 than for the Milky Way.",

keywords = "Galaxies: individual: IC 342, Galaxies: interstellar matter, ISM: general, Infrared: interstellar: lines, Radio lines: atomic, Radio lines: molecular: interstellar",

author = "B{\"u}ttgenbach, {Thomas H.} and Jocelyn Keene and Phillips, {T. G.} and Walker, {Christopher K.}",

year = "1992",

month = sep,

day = "20",

language = "English (US)",

volume = "397",

pages = "L15--L17",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 PART 2",

}

TY - JOUR

T1 - Submillimeter detection of extragalactic C I emission

T2 - IC 342

AU - Büttgenbach, Thomas H.

AU - Keene, Jocelyn

AU - Phillips, T. G.

AU - Walker, Christopher K.

PY - 1992/9/20

Y1 - 1992/9/20

N2 - We report observations of the 3P1 → 3P0 transition of atomic carbon at 492 GHz in IC 342, made at the Caltech Submillimeter Observatory, which represent the first extragalactic submillimeter detection of C I. The C I emission from IC 342 was found to have a main beam temperature of about 1 K, which is a factor of 2 greater than that for 13CO(2 → 1) in the same size beam. Comparing our data with COBE observations of the Milky Way, we find that the ratio of C I to CO(2 → 1) is approximately a factor of 2 lower in IC 342 than in our Galaxy. The result is interpreted in terms of photodissociation region models which require higher gas densities for IC 342 than for the Milky Way.

AB - We report observations of the 3P1 → 3P0 transition of atomic carbon at 492 GHz in IC 342, made at the Caltech Submillimeter Observatory, which represent the first extragalactic submillimeter detection of C I. The C I emission from IC 342 was found to have a main beam temperature of about 1 K, which is a factor of 2 greater than that for 13CO(2 → 1) in the same size beam. Comparing our data with COBE observations of the Milky Way, we find that the ratio of C I to CO(2 → 1) is approximately a factor of 2 lower in IC 342 than in our Galaxy. The result is interpreted in terms of photodissociation region models which require higher gas densities for IC 342 than for the Milky Way.

KW - Galaxies: individual: IC 342

KW - Galaxies: interstellar matter

KW - ISM: general

KW - Infrared: interstellar: lines

KW - Radio lines: atomic

KW - Radio lines: molecular: interstellar

UR - http://www.scopus.com/inward/record.url?scp=4244008235&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=4244008235&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:4244008235

SN - 0004-637X

VL - 397

SP - L15-L17

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 2

ER -

Submillimeter detection of extragalactic C I emission: IC 342

Abstract

Keywords

ASJC Scopus subject areas

Other files and links

Fingerprint

Cite this