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Title: SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690

Abstract

We have obtained high-resolution data of the z {approx} 2 ring-like, clumpy star-forming galaxy (SFG) ZC406690 using the VLT/SINFONI with adaptive optics (in K band) and in seeing-limited mode (in H and J bands). Our data include all of the main strong optical emission lines: [O II], [O III], H{alpha}, H{beta}, [N II], and [S II]. We find broad, blueshifted H{alpha} and [O III] emission line wings in the spectra of the galaxy's massive, star-forming clumps ({sigma} {approx} 85 km s{sup -1}) and even broader wings (up to 70% of the total H{alpha} flux, with {sigma} {approx} 290 km s{sup -1}) in regions spatially offset from the clumps by {approx}2 kpc. The broad emission likely originates from large-scale outflows with mass outflow rates from individual clumps that are 1-8 Multiplication-Sign the star formation rate (SFR) of the clumps. Based on emission line ratio diagnostics ([N II]/H{alpha} and [S II]/H{alpha}) and photoionization and shock models, we find that the emission from the clumps is due to a combination of photoionization from the star-forming regions and shocks generated in the outflowing component, with 5%-30% of the emission deriving from shocks. In terms of the ionization parameter (6 Multiplication-Sign 10{sup 7} to 10{supmore » 8} cm s{sup -1}, based on both the SFR and the O{sub 32} ratio), density (local electron densities of 300-1800 cm{sup -3} in and around the clumps, and ionized gas column densities of 1200-8000 M{sub Sun }pc{sup -2}), and SFR (10-40 M{sub Sun} yr{sup -1}), these clumps more closely resemble nuclear starburst regions of local ultraluminous infrared galaxies and dwarf irregulars than H II regions in local galaxies. However, the star-forming clumps are not located in the nucleus as in local starburst galaxies but instead are situated in a ring several kpc from the center of their high-redshift host galaxy, and have an overall disk-like morphology. The two brightest clumps are quite different in terms of their internal properties, energetics, and relative ages, and thus we are given a glimpse at two different stages in the formation and evolution of rapidly star-forming giant clumps at high-z.« less

Authors:
;  [1];  [2]; ; ; ; ; ; ; ; ;  [3]; ;  [4]; ;  [5];  [6];  [7];  [8];  [9] more »; « less
  1. Department of Astronomy, Campbell Hall, University of California, Berkeley, CA 94720 (United States)
  2. Aerospace Research Laboratories, Northrop Grumman Aerospace Systems, Redondo Beach, CA 90278 (United States)
  3. Max-Planck-Institut fuer extraterrestrische Physik (MPE), Giessenbachstr.1, D-85748 Garching (Germany)
  4. Institute of Astronomy, Department of Physics, Eidgenoessische Technische Hochschule, ETH Zuerich CH-8093 (Switzerland)
  5. Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, Padova I-35122 (Italy)
  6. Department of Physics and Astronomy, University of California, Santa Barbara, Santa Barbara, CA 93106 (United States)
  7. Department fuer Physik, Universitaets-Sternwarte Ludwig-Maximilians-Universitaet (USM), Scheinerstr. 1, Muenchen, D-81679 (Germany)
  8. Istituto Nazionale di AstrofisicaOsservatorio Astronomico di Arcetri, Largo Enrico Fermi 5, I 50125 Firenze (Italy)
  9. Department of Astronomy, University of Washington, Box 351580, U.W., Seattle, WA 98195-1580 (United States)
Publication Date:
OSTI Identifier:
22037017
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 752; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; DENSITY; ELECTRON DENSITY; EMISSION SPECTRA; GALACTIC EVOLUTION; MASS; MILKY WAY; NITROGEN IONS; OPTICS; OXYGEN IONS; PHOTOIONIZATION; PHOTON EMISSION; RED SHIFT; RESOLUTION; STARS; SULFUR IONS

Citation Formats

Newman, Sarah F, Genzel, Reinhard, Shapiro Griffin, Kristen, Davies, Ric, Foerster-Schreiber, Natascha M, Tacconi, Linda J, Kurk, Jaron, Wuyts, Stijn, Genel, Shy, Buschkamp, Peter, Eisenhauer, Frank, Lutz, Dieter, Lilly, Simon J, Carollo, C Marcella, Renzini, Alvio, Mancini, Chiara, Bouche, Nicolas, Burkert, Andreas, Cresci, Giovanni, Hicks, Erin, and others, and. SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690. United States: N. p., 2012. Web. doi:10.1088/0004-637X/752/2/111.
Newman, Sarah F, Genzel, Reinhard, Shapiro Griffin, Kristen, Davies, Ric, Foerster-Schreiber, Natascha M, Tacconi, Linda J, Kurk, Jaron, Wuyts, Stijn, Genel, Shy, Buschkamp, Peter, Eisenhauer, Frank, Lutz, Dieter, Lilly, Simon J, Carollo, C Marcella, Renzini, Alvio, Mancini, Chiara, Bouche, Nicolas, Burkert, Andreas, Cresci, Giovanni, Hicks, Erin, & others, and. SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690. United States. https://doi.org/10.1088/0004-637X/752/2/111
Newman, Sarah F, Genzel, Reinhard, Shapiro Griffin, Kristen, Davies, Ric, Foerster-Schreiber, Natascha M, Tacconi, Linda J, Kurk, Jaron, Wuyts, Stijn, Genel, Shy, Buschkamp, Peter, Eisenhauer, Frank, Lutz, Dieter, Lilly, Simon J, Carollo, C Marcella, Renzini, Alvio, Mancini, Chiara, Bouche, Nicolas, Burkert, Andreas, Cresci, Giovanni, Hicks, Erin, and others, and. 2012. "SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690". United States. https://doi.org/10.1088/0004-637X/752/2/111.
@article{osti_22037017,
title = {SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690},
author = {Newman, Sarah F and Genzel, Reinhard and Shapiro Griffin, Kristen and Davies, Ric and Foerster-Schreiber, Natascha M and Tacconi, Linda J and Kurk, Jaron and Wuyts, Stijn and Genel, Shy and Buschkamp, Peter and Eisenhauer, Frank and Lutz, Dieter and Lilly, Simon J and Carollo, C Marcella and Renzini, Alvio and Mancini, Chiara and Bouche, Nicolas and Burkert, Andreas and Cresci, Giovanni and Hicks, Erin and others, and},
abstractNote = {We have obtained high-resolution data of the z {approx} 2 ring-like, clumpy star-forming galaxy (SFG) ZC406690 using the VLT/SINFONI with adaptive optics (in K band) and in seeing-limited mode (in H and J bands). Our data include all of the main strong optical emission lines: [O II], [O III], H{alpha}, H{beta}, [N II], and [S II]. We find broad, blueshifted H{alpha} and [O III] emission line wings in the spectra of the galaxy's massive, star-forming clumps ({sigma} {approx} 85 km s{sup -1}) and even broader wings (up to 70% of the total H{alpha} flux, with {sigma} {approx} 290 km s{sup -1}) in regions spatially offset from the clumps by {approx}2 kpc. The broad emission likely originates from large-scale outflows with mass outflow rates from individual clumps that are 1-8 Multiplication-Sign the star formation rate (SFR) of the clumps. Based on emission line ratio diagnostics ([N II]/H{alpha} and [S II]/H{alpha}) and photoionization and shock models, we find that the emission from the clumps is due to a combination of photoionization from the star-forming regions and shocks generated in the outflowing component, with 5%-30% of the emission deriving from shocks. In terms of the ionization parameter (6 Multiplication-Sign 10{sup 7} to 10{sup 8} cm s{sup -1}, based on both the SFR and the O{sub 32} ratio), density (local electron densities of 300-1800 cm{sup -3} in and around the clumps, and ionized gas column densities of 1200-8000 M{sub Sun }pc{sup -2}), and SFR (10-40 M{sub Sun} yr{sup -1}), these clumps more closely resemble nuclear starburst regions of local ultraluminous infrared galaxies and dwarf irregulars than H II regions in local galaxies. However, the star-forming clumps are not located in the nucleus as in local starburst galaxies but instead are situated in a ring several kpc from the center of their high-redshift host galaxy, and have an overall disk-like morphology. The two brightest clumps are quite different in terms of their internal properties, energetics, and relative ages, and thus we are given a glimpse at two different stages in the formation and evolution of rapidly star-forming giant clumps at high-z.},
doi = {10.1088/0004-637X/752/2/111},
url = {https://www.osti.gov/biblio/22037017}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 752,
place = {United States},
year = {Wed Jun 20 00:00:00 EDT 2012},
month = {Wed Jun 20 00:00:00 EDT 2012}
}