Feedback in the local LBG Analog Haro 11 as probed by far-UV and X-ray observations
We have re-analyzed FUSE data and obtained new Chandra observations of Haro 11, a local (D_L=88 Mpc) UV luminous galaxy. Haro 11 has a similar far-UV luminosity (10^10.3 L_\odot), UV surface brightness (10^9.4 L_\odot kpc^-2), SFR, and metallicity to that observed in Lyman Break Galaxies (LBGs). We...
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| creator | Grimes, J P Heckman, T Strickland, D Dixon, W V Sembach, K Overzier, R Hoopes, C Aloisi, A Ptak, A |
| description | We have re-analyzed FUSE data and obtained new Chandra observations of Haro 11, a local (D_L=88 Mpc) UV luminous galaxy. Haro 11 has a similar far-UV luminosity (10^10.3 L_\odot), UV surface brightness (10^9.4 L_\odot kpc^-2), SFR, and metallicity to that observed in Lyman Break Galaxies (LBGs). We show that Haro 11 has extended, soft thermal (kT~0.68 keV) X-ray emission with a luminosity and size which scales with the physical properties (e.g. SFR, stellar mass) of the host galaxy. An enhanced alpha/Fe, ratio of ~4 relative to solar abundance suggests significant supernovae enrichment. These results are consistent with the X-ray emission being produced in a shock between a supernovae driven outflow and the ambient material. The FUV spectra show strong absorption lines similar to those observed in LBG spectra. A blueshifted absorption component is identified as a wind outflowing at ~200-280 km/s. OVI\lambda\lambda1032,1038 emission, the dominant cooling mechanism for coronal gas at T~10^5.5 K is also observed. If associated with the outflow, the luminosity of the OVI emission suggests that |
| doi_str_mv | 10.48550/arxiv.0707.0693 |
| format | Article |
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Haro 11 has a similar far-UV luminosity (10^10.3 L_\odot), UV surface brightness (10^9.4 L_\odot kpc^-2), SFR, and metallicity to that observed in Lyman Break Galaxies (LBGs). We show that Haro 11 has extended, soft thermal (kT~0.68 keV) X-ray emission with a luminosity and size which scales with the physical properties (e.g. SFR, stellar mass) of the host galaxy. An enhanced alpha/Fe, ratio of ~4 relative to solar abundance suggests significant supernovae enrichment. These results are consistent with the X-ray emission being produced in a shock between a supernovae driven outflow and the ambient material. The FUV spectra show strong absorption lines similar to those observed in LBG spectra. A blueshifted absorption component is identified as a wind outflowing at ~200-280 km/s. OVI\lambda\lambda1032,1038 emission, the dominant cooling mechanism for coronal gas at T~10^5.5 K is also observed. If associated with the outflow, the luminosity of the OVI emission suggests that <20% of the total mechanical energy from the supernovae and solar winds is being radiated away. This implies that radiative cooling through OVI is not significantly inhibiting the growth of the outflowing gas. In contradiction to the findings of Bergvall et al 2006, we find no convincing evidence of Lyman continuum leakage in Haro 11. We conclude that the wind has not created a `tunnel' allowing the escape of a significant fraction of Lyman continuum photons and place a limit on the escape fraction of f_{esc}<2%. Overall, both Haro 11 and a previously observed LBG analogue VV 114, provide an invaluable insight into the X-ray and FUV properties of high redshift LBGs.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.0707.0693</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Absorption ; Abundance ; Cooling ; Coronas ; Emission ; Galaxies ; Line spectra ; Luminosity ; Metallicity ; Outflow ; Photons ; Physical properties ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Red shift ; Stellar mass ; Stellar winds ; Supernovae ; Surface brightness</subject><ispartof>arXiv.org, 2007-07</ispartof><rights>Notwithstanding the ProQuest Terms and conditions, you may use this content in accordance with the associated terms available at http://arxiv.org/abs/0707.0693.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.0707.0693$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1086/521353$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Grimes, J P</creatorcontrib><creatorcontrib>Heckman, T</creatorcontrib><creatorcontrib>Strickland, D</creatorcontrib><creatorcontrib>Dixon, W V</creatorcontrib><creatorcontrib>Sembach, K</creatorcontrib><creatorcontrib>Overzier, R</creatorcontrib><creatorcontrib>Hoopes, C</creatorcontrib><creatorcontrib>Aloisi, A</creatorcontrib><creatorcontrib>Ptak, A</creatorcontrib><title>Feedback in the local LBG Analog Haro 11 as probed by far-UV and X-ray observations</title><title>arXiv.org</title><description>We have re-analyzed FUSE data and obtained new Chandra observations of Haro 11, a local (D_L=88 Mpc) UV luminous galaxy. Haro 11 has a similar far-UV luminosity (10^10.3 L_\odot), UV surface brightness (10^9.4 L_\odot kpc^-2), SFR, and metallicity to that observed in Lyman Break Galaxies (LBGs). We show that Haro 11 has extended, soft thermal (kT~0.68 keV) X-ray emission with a luminosity and size which scales with the physical properties (e.g. SFR, stellar mass) of the host galaxy. An enhanced alpha/Fe, ratio of ~4 relative to solar abundance suggests significant supernovae enrichment. These results are consistent with the X-ray emission being produced in a shock between a supernovae driven outflow and the ambient material. The FUV spectra show strong absorption lines similar to those observed in LBG spectra. A blueshifted absorption component is identified as a wind outflowing at ~200-280 km/s. OVI\lambda\lambda1032,1038 emission, the dominant cooling mechanism for coronal gas at T~10^5.5 K is also observed. If associated with the outflow, the luminosity of the OVI emission suggests that <20% of the total mechanical energy from the supernovae and solar winds is being radiated away. This implies that radiative cooling through OVI is not significantly inhibiting the growth of the outflowing gas. In contradiction to the findings of Bergvall et al 2006, we find no convincing evidence of Lyman continuum leakage in Haro 11. We conclude that the wind has not created a `tunnel' allowing the escape of a significant fraction of Lyman continuum photons and place a limit on the escape fraction of f_{esc}<2%. Overall, both Haro 11 and a previously observed LBG analogue VV 114, provide an invaluable insight into the X-ray and FUV properties of high redshift LBGs.</description><subject>Absorption</subject><subject>Abundance</subject><subject>Cooling</subject><subject>Coronas</subject><subject>Emission</subject><subject>Galaxies</subject><subject>Line spectra</subject><subject>Luminosity</subject><subject>Metallicity</subject><subject>Outflow</subject><subject>Photons</subject><subject>Physical properties</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Red shift</subject><subject>Stellar mass</subject><subject>Stellar winds</subject><subject>Supernovae</subject><subject>Surface brightness</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj0FPwkAQhTcmJhLk7slM4rk43e22u0ckAiYkHkTjrZltBy3WLu4CkX9vUU_vHb68vE-IqxTHmdEabyl8N4cxFliMMbfqTAykUmliMikvxCjGDSLKvJBaq4F4mjHXjqoPaDrYvTO0vqIWlndzmHTU-jdYUPCQpkARtsE7rsEdYU0heX4B6mp4TQIdwbvI4UC7xnfxUpyvqY08-s-hWM3uV9NFsnycP0wny4R0qhKJlLJmU-dcFWiy3LGtMsOyYq2z1PbNSaucRWUtaSZcW6m0yTkzNRtUQ3H9N_srXG5D80nhWJ7Ey5N4D9z8Af3vrz3HXbnx-9BbxVKiscZiUSj1A64gWHg</recordid><startdate>20070704</startdate><enddate>20070704</enddate><creator>Grimes, J P</creator><creator>Heckman, T</creator><creator>Strickland, D</creator><creator>Dixon, W V</creator><creator>Sembach, K</creator><creator>Overzier, R</creator><creator>Hoopes, C</creator><creator>Aloisi, A</creator><creator>Ptak, A</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20070704</creationdate><title>Feedback in the local LBG Analog Haro 11 as probed by far-UV and X-ray observations</title><author>Grimes, J P ; Heckman, T ; Strickland, D ; Dixon, W V ; Sembach, K ; Overzier, R ; Hoopes, C ; Aloisi, A ; Ptak, A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a513-20a1e5e8d6ec70846be9c48e2ce554198e2b293b90399a5ea0f923586e48de803</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2007</creationdate><topic>Absorption</topic><topic>Abundance</topic><topic>Cooling</topic><topic>Coronas</topic><topic>Emission</topic><topic>Galaxies</topic><topic>Line spectra</topic><topic>Luminosity</topic><topic>Metallicity</topic><topic>Outflow</topic><topic>Photons</topic><topic>Physical properties</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Red shift</topic><topic>Stellar mass</topic><topic>Stellar winds</topic><topic>Supernovae</topic><topic>Surface brightness</topic><toplevel>online_resources</toplevel><creatorcontrib>Grimes, J P</creatorcontrib><creatorcontrib>Heckman, T</creatorcontrib><creatorcontrib>Strickland, D</creatorcontrib><creatorcontrib>Dixon, W V</creatorcontrib><creatorcontrib>Sembach, K</creatorcontrib><creatorcontrib>Overzier, R</creatorcontrib><creatorcontrib>Hoopes, C</creatorcontrib><creatorcontrib>Aloisi, A</creatorcontrib><creatorcontrib>Ptak, A</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Grimes, J P</au><au>Heckman, T</au><au>Strickland, D</au><au>Dixon, W V</au><au>Sembach, K</au><au>Overzier, R</au><au>Hoopes, C</au><au>Aloisi, A</au><au>Ptak, A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Feedback in the local LBG Analog Haro 11 as probed by far-UV and X-ray observations</atitle><jtitle>arXiv.org</jtitle><date>2007-07-04</date><risdate>2007</risdate><eissn>2331-8422</eissn><abstract>We have re-analyzed FUSE data and obtained new Chandra observations of Haro 11, a local (D_L=88 Mpc) UV luminous galaxy. Haro 11 has a similar far-UV luminosity (10^10.3 L_\odot), UV surface brightness (10^9.4 L_\odot kpc^-2), SFR, and metallicity to that observed in Lyman Break Galaxies (LBGs). We show that Haro 11 has extended, soft thermal (kT~0.68 keV) X-ray emission with a luminosity and size which scales with the physical properties (e.g. SFR, stellar mass) of the host galaxy. An enhanced alpha/Fe, ratio of ~4 relative to solar abundance suggests significant supernovae enrichment. These results are consistent with the X-ray emission being produced in a shock between a supernovae driven outflow and the ambient material. The FUV spectra show strong absorption lines similar to those observed in LBG spectra. A blueshifted absorption component is identified as a wind outflowing at ~200-280 km/s. OVI\lambda\lambda1032,1038 emission, the dominant cooling mechanism for coronal gas at T~10^5.5 K is also observed. If associated with the outflow, the luminosity of the OVI emission suggests that <20% of the total mechanical energy from the supernovae and solar winds is being radiated away. This implies that radiative cooling through OVI is not significantly inhibiting the growth of the outflowing gas. In contradiction to the findings of Bergvall et al 2006, we find no convincing evidence of Lyman continuum leakage in Haro 11. We conclude that the wind has not created a `tunnel' allowing the escape of a significant fraction of Lyman continuum photons and place a limit on the escape fraction of f_{esc}<2%. Overall, both Haro 11 and a previously observed LBG analogue VV 114, provide an invaluable insight into the X-ray and FUV properties of high redshift LBGs.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.0707.0693</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Absorption Abundance Cooling Coronas Emission Galaxies Line spectra Luminosity Metallicity Outflow Photons Physical properties Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics Red shift Stellar mass Stellar winds Supernovae Surface brightness |
| title | Feedback in the local LBG Analog Haro 11 as probed by far-UV and X-ray observations |
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