Large-scale shock-ionized and photoionized gas in M83: The impact of star formation

Sungryong Hong, Daniela Calzetti, Michael A. Dopita, William P. Blair, Bradley C. Whitmore, Bruce Balick, Howard E. Bond, Marcella Carollo, Michael J. Disney, Jay A. Frogel, Donald Hall, Jon A. Holtzman, Randy A. Kimble, Patrick J. McCarthy, Robert W. O'Connell, Francesco Paresce, Abhijit Saha, Joseph I. Silk, John T. Trauger, Alistair R. WalkerRogier Windhorst, Erick T. Young, Max Mutchler

Research output: Contribution to journalArticle

10 Citations (Scopus)

Abstract

We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007)/Hβ versus [S II](6716+6731)/ Hα, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (02 × 02) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/Hβ) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized Hα emission ranges from ∼2% to about 15%-33% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/Hβ) 0. This feature is well fit by a shock-ionization model with 2.0 Z metallicity and shock velocities in the range of 250-350 km s-1. A low-velocity shock component, <200 km s-1, is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33% of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83.

Original languageEnglish (US)
Article number45
JournalAstrophysical Journal
Volume731
Issue number1
DOIs
StatePublished - Apr 10 2011

Fingerprint

ionized gases
star formation
diagram
shock
diagrams
gases
gas
ionization
pixel
Hubble Space Telescope
low speed
metallicity
pixels
horizontal distribution
rings
H II regions
extinction
supernova remnants
dust
narrowband

Keywords

  • galaxies: interactions
  • galaxies: ISM
  • galaxies: starburst
  • ISM: structure

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Hong, S., Calzetti, D., Dopita, M. A., Blair, W. P., Whitmore, B. C., Balick, B., ... Mutchler, M. (2011). Large-scale shock-ionized and photoionized gas in M83: The impact of star formation. Astrophysical Journal, 731(1), [45]. https://doi.org/10.1088/0004-637X/731/1/45

Large-scale shock-ionized and photoionized gas in M83 : The impact of star formation. / Hong, Sungryong; Calzetti, Daniela; Dopita, Michael A.; Blair, William P.; Whitmore, Bradley C.; Balick, Bruce; Bond, Howard E.; Carollo, Marcella; Disney, Michael J.; Frogel, Jay A.; Hall, Donald; Holtzman, Jon A.; Kimble, Randy A.; McCarthy, Patrick J.; O'Connell, Robert W.; Paresce, Francesco; Saha, Abhijit; Silk, Joseph I.; Trauger, John T.; Walker, Alistair R.; Windhorst, Rogier; Young, Erick T.; Mutchler, Max.

In: Astrophysical Journal, Vol. 731, No. 1, 45, 10.04.2011.

Research output: Contribution to journalArticle

Hong, S, Calzetti, D, Dopita, MA, Blair, WP, Whitmore, BC, Balick, B, Bond, HE, Carollo, M, Disney, MJ, Frogel, JA, Hall, D, Holtzman, JA, Kimble, RA, McCarthy, PJ, O'Connell, RW, Paresce, F, Saha, A, Silk, JI, Trauger, JT, Walker, AR, Windhorst, R, Young, ET & Mutchler, M 2011, 'Large-scale shock-ionized and photoionized gas in M83: The impact of star formation', Astrophysical Journal, vol. 731, no. 1, 45. https://doi.org/10.1088/0004-637X/731/1/45
Hong S, Calzetti D, Dopita MA, Blair WP, Whitmore BC, Balick B et al. Large-scale shock-ionized and photoionized gas in M83: The impact of star formation. Astrophysical Journal. 2011 Apr 10;731(1). 45. https://doi.org/10.1088/0004-637X/731/1/45
Hong, Sungryong ; Calzetti, Daniela ; Dopita, Michael A. ; Blair, William P. ; Whitmore, Bradley C. ; Balick, Bruce ; Bond, Howard E. ; Carollo, Marcella ; Disney, Michael J. ; Frogel, Jay A. ; Hall, Donald ; Holtzman, Jon A. ; Kimble, Randy A. ; McCarthy, Patrick J. ; O'Connell, Robert W. ; Paresce, Francesco ; Saha, Abhijit ; Silk, Joseph I. ; Trauger, John T. ; Walker, Alistair R. ; Windhorst, Rogier ; Young, Erick T. ; Mutchler, Max. / Large-scale shock-ionized and photoionized gas in M83 : The impact of star formation. In: Astrophysical Journal. 2011 ; Vol. 731, No. 1.
@article{e57a51943b904994a0552aed7d2d05a1,
title = "Large-scale shock-ionized and photoionized gas in M83: The impact of star formation",
abstract = "We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007)/Hβ versus [S II](6716+6731)/ Hα, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (02 × 02) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/Hβ) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized Hα emission ranges from ∼2{\%} to about 15{\%}-33{\%} of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/Hβ) 0. This feature is well fit by a shock-ionization model with 2.0 Z metallicity and shock velocities in the range of 250-350 km s-1. A low-velocity shock component, <200 km s-1, is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33{\%} of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83.",
keywords = "galaxies: interactions, galaxies: ISM, galaxies: starburst, ISM: structure",
author = "Sungryong Hong and Daniela Calzetti and Dopita, {Michael A.} and Blair, {William P.} and Whitmore, {Bradley C.} and Bruce Balick and Bond, {Howard E.} and Marcella Carollo and Disney, {Michael J.} and Frogel, {Jay A.} and Donald Hall and Holtzman, {Jon A.} and Kimble, {Randy A.} and McCarthy, {Patrick J.} and O'Connell, {Robert W.} and Francesco Paresce and Abhijit Saha and Silk, {Joseph I.} and Trauger, {John T.} and Walker, {Alistair R.} and Rogier Windhorst and Young, {Erick T.} and Max Mutchler",
year = "2011",
month = "4",
day = "10",
doi = "10.1088/0004-637X/731/1/45",
language = "English (US)",
volume = "731",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - Large-scale shock-ionized and photoionized gas in M83

T2 - The impact of star formation

AU - Hong, Sungryong

AU - Calzetti, Daniela

AU - Dopita, Michael A.

AU - Blair, William P.

AU - Whitmore, Bradley C.

AU - Balick, Bruce

AU - Bond, Howard E.

AU - Carollo, Marcella

AU - Disney, Michael J.

AU - Frogel, Jay A.

AU - Hall, Donald

AU - Holtzman, Jon A.

AU - Kimble, Randy A.

AU - McCarthy, Patrick J.

AU - O'Connell, Robert W.

AU - Paresce, Francesco

AU - Saha, Abhijit

AU - Silk, Joseph I.

AU - Trauger, John T.

AU - Walker, Alistair R.

AU - Windhorst, Rogier

AU - Young, Erick T.

AU - Mutchler, Max

PY - 2011/4/10

Y1 - 2011/4/10

N2 - We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007)/Hβ versus [S II](6716+6731)/ Hα, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (02 × 02) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/Hβ) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized Hα emission ranges from ∼2% to about 15%-33% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/Hβ) 0. This feature is well fit by a shock-ionization model with 2.0 Z metallicity and shock velocities in the range of 250-350 km s-1. A low-velocity shock component, <200 km s-1, is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33% of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83.

AB - We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007)/Hβ versus [S II](6716+6731)/ Hα, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (02 × 02) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/Hβ) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized Hα emission ranges from ∼2% to about 15%-33% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/Hβ) 0. This feature is well fit by a shock-ionization model with 2.0 Z metallicity and shock velocities in the range of 250-350 km s-1. A low-velocity shock component, <200 km s-1, is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33% of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83.

KW - galaxies: interactions

KW - galaxies: ISM

KW - galaxies: starburst

KW - ISM: structure

UR - http://www.scopus.com/inward/record.url?scp=79955009085&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=79955009085&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/731/1/45

DO - 10.1088/0004-637X/731/1/45

M3 - Article

AN - SCOPUS:79955009085

VL - 731

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 45

ER -