A near-infrared survey of radio-selected ultracompact H II regions

M. M. Hanson, K. L. Luhman, George H. Rieke

Research output: Contribution to journalArticle

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Abstract

A near-infrared (NIR) survey of 63 radio-selected, ultracompact (UC) H II regions representing 47 different star-forming sites has been completed. The survey was obtained using H-band imaging and moderate-resolution, R = 1200, K-band spectroscopy, centered on the radio emission peak of the UC H II regions. The goal of this survey was to determine the fraction of radio-selected UC H II regions that can be studied with NIR observations and analysis. Approximately 50% of the 63 radio-selected UC H II regions appear to be detected at NIR wavelengths in Brγ emission (107 ergs s -1 cm-2 sr-1). Typical line-of-sight extinction toward the detected UC H II regions ranged from AV = 30 to 50, though one source was measured to have AV = 80. For a few of these UC H II regions, the central ionizing sources are detected through high signal-to-noise ratio NIR spectra of photospheric transitions. This preliminary survey suggests that perhaps 5%-10% of UC H II regions showing NIR counterparts will have directly detectable central ionizing sources. Using the ratio of He I 2.11 to Brγ, the effective temperatures of the central ionizing stars in 25 UC H II regions have been estimated. While He I is not always detected in UC H II regions, when it was found or a meaningful upper limit determined, the spectral type implied by the ratio of He I 2.11 to Brγ closely matched similar estimates of spectral type derived from radio. Model predictions based on mid-infrared measurements appear to underestimate the temperature of the central ionizing stars for which we have directly detected spectral types. The line ratios of H2 2-1 S(1) and 1-0 S(0) relative to the 1-0 S(1) line in our sample of UC H II regions are generally indicative of dense photodissociation regions rather than shocks, similar to what is seen in the Orion Bar. This was true even for UC H II regions showing very weak Brγ emission. While Brγ was generally found to be spatially correlated with the radio emission, H2 showed little correlation with the UC H II regions, typically lying ≳ 10″ from the central radio emission. A discussion of each UC H II region studied is included in an extensive appendix.

Original languageEnglish (US)
Pages (from-to)35-61
Number of pages27
JournalAstrophysical Journal, Supplement Series
Volume138
Issue number1
DOIs
StatePublished - Jan 1 2002

Fingerprint

H II regions
near infrared
radio
radio emission
stars
extremely high frequencies
photodissociation
line of sight
erg
signal-to-noise ratio
extinction
signal to noise ratios
infrared spectra
shock

Keywords

  • H II regions
  • Infrared: ISM
  • ISM: lines and bands
  • ISM: molecules
  • Stars: evolution
  • Stars: formation

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

A near-infrared survey of radio-selected ultracompact H II regions. / Hanson, M. M.; Luhman, K. L.; Rieke, George H.

In: Astrophysical Journal, Supplement Series, Vol. 138, No. 1, 01.01.2002, p. 35-61.

Research output: Contribution to journalArticle

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abstract = "A near-infrared (NIR) survey of 63 radio-selected, ultracompact (UC) H II regions representing 47 different star-forming sites has been completed. The survey was obtained using H-band imaging and moderate-resolution, R = 1200, K-band spectroscopy, centered on the radio emission peak of the UC H II regions. The goal of this survey was to determine the fraction of radio-selected UC H II regions that can be studied with NIR observations and analysis. Approximately 50{\%} of the 63 radio-selected UC H II regions appear to be detected at NIR wavelengths in Brγ emission (107 ergs s -1 cm-2 sr-1). Typical line-of-sight extinction toward the detected UC H II regions ranged from AV = 30 to 50, though one source was measured to have AV = 80. For a few of these UC H II regions, the central ionizing sources are detected through high signal-to-noise ratio NIR spectra of photospheric transitions. This preliminary survey suggests that perhaps 5{\%}-10{\%} of UC H II regions showing NIR counterparts will have directly detectable central ionizing sources. Using the ratio of He I 2.11 to Brγ, the effective temperatures of the central ionizing stars in 25 UC H II regions have been estimated. While He I is not always detected in UC H II regions, when it was found or a meaningful upper limit determined, the spectral type implied by the ratio of He I 2.11 to Brγ closely matched similar estimates of spectral type derived from radio. Model predictions based on mid-infrared measurements appear to underestimate the temperature of the central ionizing stars for which we have directly detected spectral types. The line ratios of H2 2-1 S(1) and 1-0 S(0) relative to the 1-0 S(1) line in our sample of UC H II regions are generally indicative of dense photodissociation regions rather than shocks, similar to what is seen in the Orion Bar. This was true even for UC H II regions showing very weak Brγ emission. While Brγ was generally found to be spatially correlated with the radio emission, H2 showed little correlation with the UC H II regions, typically lying ≳ 10″ from the central radio emission. A discussion of each UC H II region studied is included in an extensive appendix.",
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N2 - A near-infrared (NIR) survey of 63 radio-selected, ultracompact (UC) H II regions representing 47 different star-forming sites has been completed. The survey was obtained using H-band imaging and moderate-resolution, R = 1200, K-band spectroscopy, centered on the radio emission peak of the UC H II regions. The goal of this survey was to determine the fraction of radio-selected UC H II regions that can be studied with NIR observations and analysis. Approximately 50% of the 63 radio-selected UC H II regions appear to be detected at NIR wavelengths in Brγ emission (107 ergs s -1 cm-2 sr-1). Typical line-of-sight extinction toward the detected UC H II regions ranged from AV = 30 to 50, though one source was measured to have AV = 80. For a few of these UC H II regions, the central ionizing sources are detected through high signal-to-noise ratio NIR spectra of photospheric transitions. This preliminary survey suggests that perhaps 5%-10% of UC H II regions showing NIR counterparts will have directly detectable central ionizing sources. Using the ratio of He I 2.11 to Brγ, the effective temperatures of the central ionizing stars in 25 UC H II regions have been estimated. While He I is not always detected in UC H II regions, when it was found or a meaningful upper limit determined, the spectral type implied by the ratio of He I 2.11 to Brγ closely matched similar estimates of spectral type derived from radio. Model predictions based on mid-infrared measurements appear to underestimate the temperature of the central ionizing stars for which we have directly detected spectral types. The line ratios of H2 2-1 S(1) and 1-0 S(0) relative to the 1-0 S(1) line in our sample of UC H II regions are generally indicative of dense photodissociation regions rather than shocks, similar to what is seen in the Orion Bar. This was true even for UC H II regions showing very weak Brγ emission. While Brγ was generally found to be spatially correlated with the radio emission, H2 showed little correlation with the UC H II regions, typically lying ≳ 10″ from the central radio emission. A discussion of each UC H II region studied is included in an extensive appendix.

AB - A near-infrared (NIR) survey of 63 radio-selected, ultracompact (UC) H II regions representing 47 different star-forming sites has been completed. The survey was obtained using H-band imaging and moderate-resolution, R = 1200, K-band spectroscopy, centered on the radio emission peak of the UC H II regions. The goal of this survey was to determine the fraction of radio-selected UC H II regions that can be studied with NIR observations and analysis. Approximately 50% of the 63 radio-selected UC H II regions appear to be detected at NIR wavelengths in Brγ emission (107 ergs s -1 cm-2 sr-1). Typical line-of-sight extinction toward the detected UC H II regions ranged from AV = 30 to 50, though one source was measured to have AV = 80. For a few of these UC H II regions, the central ionizing sources are detected through high signal-to-noise ratio NIR spectra of photospheric transitions. This preliminary survey suggests that perhaps 5%-10% of UC H II regions showing NIR counterparts will have directly detectable central ionizing sources. Using the ratio of He I 2.11 to Brγ, the effective temperatures of the central ionizing stars in 25 UC H II regions have been estimated. While He I is not always detected in UC H II regions, when it was found or a meaningful upper limit determined, the spectral type implied by the ratio of He I 2.11 to Brγ closely matched similar estimates of spectral type derived from radio. Model predictions based on mid-infrared measurements appear to underestimate the temperature of the central ionizing stars for which we have directly detected spectral types. The line ratios of H2 2-1 S(1) and 1-0 S(0) relative to the 1-0 S(1) line in our sample of UC H II regions are generally indicative of dense photodissociation regions rather than shocks, similar to what is seen in the Orion Bar. This was true even for UC H II regions showing very weak Brγ emission. While Brγ was generally found to be spatially correlated with the radio emission, H2 showed little correlation with the UC H II regions, typically lying ≳ 10″ from the central radio emission. A discussion of each UC H II region studied is included in an extensive appendix.

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KW - Infrared: ISM

KW - ISM: lines and bands

KW - ISM: molecules

KW - Stars: evolution

KW - Stars: formation

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