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The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift
We present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 m emission in four z ∼ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 m (observed 345 GHz) dust emission is...
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| Published in: | The Astrophysical journal 2018-05, Vol.859 (1), p.12 |
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| creator | Gullberg, B. Swinbank, A. M. Smail, I. Biggs, A. D. Bertoldi, F. Breuck, C. De Chapman, S. C. Chen, C.-C. Cooke, E. A. Coppin, K. E. K. Cox, P. Dannerbauer, H. Dunlop, J. S. Edge, A. C. Farrah, D. Geach, J. E. Greve, T. R. Hodge, J. Ibar, E. Ivison, R. J. Karim, A. Schinnerer, E. Scott, D. Simpson, J. M. Stach, S. M. Thomson, A. P. van der Werf, P. Walter, F. Wardlow, J. L. Weiss, A. |
| description | We present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 m emission in four z ∼ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations ( Jy beam−1). The four SMGs are bright [C ii] emitters. We extract [C ii] spectra from the high-resolution data, and recover ∼20%-100% of the [C ii] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C ii] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 m dust continuum by a factor of 1.6 0.4. By considering the / ratio as a function of the star formation rate surface density ( ), we revisit the [C ii] deficit and suggest that the decline in the / ratio as a function of is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs. |
| doi_str_mv | 10.3847/1538-4357/aabe8c |
| format | article |
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L. ; Weiss, A.</creatorcontrib><description>We present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 m emission in four z ∼ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations ( Jy beam−1). The four SMGs are bright [C ii] emitters. We extract [C ii] spectra from the high-resolution data, and recover ∼20%-100% of the [C ii] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C ii] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 m dust continuum by a factor of 1.6 0.4. By considering the / ratio as a function of the star formation rate surface density ( ), we revisit the [C ii] deficit and suggest that the decline in the / ratio as a function of is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aabe8c</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Angular resolution ; Astrophysics ; Clumps ; Continuum radiation ; Cosmic dust ; Disks ; Dust ; Dust emission ; Emission ; Emitters ; Galaxies ; galaxies: evolution ; galaxies: ISM ; High resolution ; Interstellar matter ; Interstellar medium ; Morphology ; Red shift ; Sciences of the Universe ; Spectral emittance ; Star & galaxy formation ; Star formation ; Star formation rate ; Stars & galaxies ; submillimeter: galaxies ; Substructures</subject><ispartof>The Astrophysical journal, 2018-05, Vol.859 (1), p.12</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing May 20, 2018</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c394c-e255fcdd36ba25b022da456c23fd28f753ea7f5e32a99804d2027df061e13bc73</citedby><cites>FETCH-LOGICAL-c394c-e255fcdd36ba25b022da456c23fd28f753ea7f5e32a99804d2027df061e13bc73</cites><orcidid>0000-0002-3805-0789 ; 0000-0002-6878-9840 ; 0000-0003-1122-6948 ; 0000-0003-1192-5837 ; 0000-0002-8414-9579 ; 0000-0003-3843-8393 ; 0000-0001-5118-1313 ; 0000-0002-8521-1995 ; 0000-0002-3933-7677 ; 0000-0002-3398-6916 ; 0000-0002-2554-1837 ; 0000-0002-1707-1775 ; 0000-0003-3037-257X ; 0000-0003-4793-7880 ; 0000-0002-0729-2988 ; 0000-0001-7147-3575 ; 0000-0003-2376-8971 ; 0000-0003-1748-2010 ; 0000-0001-6586-8845 ; 0000-0003-4678-3939 ; 0000-0003-2027-8221 ; 0000-0001-5434-5942</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,315,786,790,891,27957,27958</link.rule.ids><backlink>$$Uhttps://hal.science/hal-02375607$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Gullberg, B.</creatorcontrib><creatorcontrib>Swinbank, A. M.</creatorcontrib><creatorcontrib>Smail, I.</creatorcontrib><creatorcontrib>Biggs, A. D.</creatorcontrib><creatorcontrib>Bertoldi, F.</creatorcontrib><creatorcontrib>Breuck, C. De</creatorcontrib><creatorcontrib>Chapman, S. C.</creatorcontrib><creatorcontrib>Chen, C.-C.</creatorcontrib><creatorcontrib>Cooke, E. A.</creatorcontrib><creatorcontrib>Coppin, K. E. K.</creatorcontrib><creatorcontrib>Cox, P.</creatorcontrib><creatorcontrib>Dannerbauer, H.</creatorcontrib><creatorcontrib>Dunlop, J. S.</creatorcontrib><creatorcontrib>Edge, A. C.</creatorcontrib><creatorcontrib>Farrah, D.</creatorcontrib><creatorcontrib>Geach, J. E.</creatorcontrib><creatorcontrib>Greve, T. R.</creatorcontrib><creatorcontrib>Hodge, J.</creatorcontrib><creatorcontrib>Ibar, E.</creatorcontrib><creatorcontrib>Ivison, R. J.</creatorcontrib><creatorcontrib>Karim, A.</creatorcontrib><creatorcontrib>Schinnerer, E.</creatorcontrib><creatorcontrib>Scott, D.</creatorcontrib><creatorcontrib>Simpson, J. M.</creatorcontrib><creatorcontrib>Stach, S. M.</creatorcontrib><creatorcontrib>Thomson, A. P.</creatorcontrib><creatorcontrib>van der Werf, P.</creatorcontrib><creatorcontrib>Walter, F.</creatorcontrib><creatorcontrib>Wardlow, J. L.</creatorcontrib><creatorcontrib>Weiss, A.</creatorcontrib><title>The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 m emission in four z ∼ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations ( Jy beam−1). The four SMGs are bright [C ii] emitters. We extract [C ii] spectra from the high-resolution data, and recover ∼20%-100% of the [C ii] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C ii] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 m dust continuum by a factor of 1.6 0.4. By considering the / ratio as a function of the star formation rate surface density ( ), we revisit the [C ii] deficit and suggest that the decline in the / ratio as a function of is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.</description><subject>Angular resolution</subject><subject>Astrophysics</subject><subject>Clumps</subject><subject>Continuum radiation</subject><subject>Cosmic dust</subject><subject>Disks</subject><subject>Dust</subject><subject>Dust emission</subject><subject>Emission</subject><subject>Emitters</subject><subject>Galaxies</subject><subject>galaxies: evolution</subject><subject>galaxies: ISM</subject><subject>High resolution</subject><subject>Interstellar matter</subject><subject>Interstellar medium</subject><subject>Morphology</subject><subject>Red shift</subject><subject>Sciences of the Universe</subject><subject>Spectral emittance</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Star formation rate</subject><subject>Stars & galaxies</subject><subject>submillimeter: galaxies</subject><subject>Substructures</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kd9q1TAcx4M48Di99zKgN4Ld0qRpWu8OR7czOGMwJwgiIc2f0xzSpiatuDfwYXwEn8YnsVnHvNGrkF8-388v8AXgRY5OSFWw05ySKisIZadCNLqSj8DqYfQYrBBCRVYS9ukJeBrjIV1xXa_Az5tWw3dTHKHoFfy8gdZ-gZc-DK13fm91hN7Aa61ia80If__4VZxQ-GFqss46Zzs96gDPhRPfEyruCIwQHOQcit5No_X9W5iWrJuoe6mTbyfCXsONm7ohQtvDcX6-6GdVHLVzIsBLrezUJd_W7tss3O9_Bo6McFE_vz-Pwcez9zebbba7Or_YrHeZJHUhM40pNVIpUjYC0wZhrERBS4mJUbgyjBItmKGaYFHXFSoURpgpg8pc56SRjByD14u3FY4PwXYi3HIvLN-udzzNECaMloh9y2f25cIOwX-ddBz5wU-hn7_HMSlpjRlFdKbQQsngYwzaPGhzxFN_PJXFU1l86W-OvFoi1g9_nWI48IrWPOc55oMyM_bmH9h_rX8AaK2q4g</recordid><startdate>20180520</startdate><enddate>20180520</enddate><creator>Gullberg, B.</creator><creator>Swinbank, A. 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L.</creator><creator>Weiss, A.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><orcidid>https://orcid.org/0000-0002-3805-0789</orcidid><orcidid>https://orcid.org/0000-0002-6878-9840</orcidid><orcidid>https://orcid.org/0000-0003-1122-6948</orcidid><orcidid>https://orcid.org/0000-0003-1192-5837</orcidid><orcidid>https://orcid.org/0000-0002-8414-9579</orcidid><orcidid>https://orcid.org/0000-0003-3843-8393</orcidid><orcidid>https://orcid.org/0000-0001-5118-1313</orcidid><orcidid>https://orcid.org/0000-0002-8521-1995</orcidid><orcidid>https://orcid.org/0000-0002-3933-7677</orcidid><orcidid>https://orcid.org/0000-0002-3398-6916</orcidid><orcidid>https://orcid.org/0000-0002-2554-1837</orcidid><orcidid>https://orcid.org/0000-0002-1707-1775</orcidid><orcidid>https://orcid.org/0000-0003-3037-257X</orcidid><orcidid>https://orcid.org/0000-0003-4793-7880</orcidid><orcidid>https://orcid.org/0000-0002-0729-2988</orcidid><orcidid>https://orcid.org/0000-0001-7147-3575</orcidid><orcidid>https://orcid.org/0000-0003-2376-8971</orcidid><orcidid>https://orcid.org/0000-0003-1748-2010</orcidid><orcidid>https://orcid.org/0000-0001-6586-8845</orcidid><orcidid>https://orcid.org/0000-0003-4678-3939</orcidid><orcidid>https://orcid.org/0000-0003-2027-8221</orcidid><orcidid>https://orcid.org/0000-0001-5434-5942</orcidid></search><sort><creationdate>20180520</creationdate><title>The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift</title><author>Gullberg, B. ; Swinbank, A. M. ; Smail, I. ; Biggs, A. D. ; Bertoldi, F. ; Breuck, C. De ; Chapman, S. C. ; Chen, C.-C. ; Cooke, E. A. ; Coppin, K. E. K. ; Cox, P. ; Dannerbauer, H. ; Dunlop, J. S. ; Edge, A. C. ; Farrah, D. ; Geach, J. E. ; Greve, T. R. ; Hodge, J. ; Ibar, E. ; Ivison, R. J. ; Karim, A. ; Schinnerer, E. ; Scott, D. ; Simpson, J. M. ; Stach, S. M. ; Thomson, A. P. ; van der Werf, P. ; Walter, F. ; Wardlow, J. 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M.</creatorcontrib><creatorcontrib>Stach, S. M.</creatorcontrib><creatorcontrib>Thomson, A. P.</creatorcontrib><creatorcontrib>van der Werf, P.</creatorcontrib><creatorcontrib>Walter, F.</creatorcontrib><creatorcontrib>Wardlow, J. L.</creatorcontrib><creatorcontrib>Weiss, A.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Gullberg, B.</au><au>Swinbank, A. M.</au><au>Smail, I.</au><au>Biggs, A. D.</au><au>Bertoldi, F.</au><au>Breuck, C. De</au><au>Chapman, S. C.</au><au>Chen, C.-C.</au><au>Cooke, E. A.</au><au>Coppin, K. E. K.</au><au>Cox, P.</au><au>Dannerbauer, H.</au><au>Dunlop, J. S.</au><au>Edge, A. C.</au><au>Farrah, D.</au><au>Geach, J. E.</au><au>Greve, T. R.</au><au>Hodge, J.</au><au>Ibar, E.</au><au>Ivison, R. J.</au><au>Karim, A.</au><au>Schinnerer, E.</au><au>Scott, D.</au><au>Simpson, J. M.</au><au>Stach, S. M.</au><au>Thomson, A. P.</au><au>van der Werf, P.</au><au>Walter, F.</au><au>Wardlow, J. L.</au><au>Weiss, A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-05-20</date><risdate>2018</risdate><volume>859</volume><issue>1</issue><spage>12</spage><pages>12-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><notes>Galaxies and Cosmology</notes><notes>AAS07434</notes><abstract>We present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 m emission in four z ∼ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations ( Jy beam−1). The four SMGs are bright [C ii] emitters. We extract [C ii] spectra from the high-resolution data, and recover ∼20%-100% of the [C ii] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C ii] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 m dust continuum by a factor of 1.6 0.4. By considering the / ratio as a function of the star formation rate surface density ( ), we revisit the [C ii] deficit and suggest that the decline in the / ratio as a function of is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aabe8c</doi><orcidid>https://orcid.org/0000-0002-3805-0789</orcidid><orcidid>https://orcid.org/0000-0002-6878-9840</orcidid><orcidid>https://orcid.org/0000-0003-1122-6948</orcidid><orcidid>https://orcid.org/0000-0003-1192-5837</orcidid><orcidid>https://orcid.org/0000-0002-8414-9579</orcidid><orcidid>https://orcid.org/0000-0003-3843-8393</orcidid><orcidid>https://orcid.org/0000-0001-5118-1313</orcidid><orcidid>https://orcid.org/0000-0002-8521-1995</orcidid><orcidid>https://orcid.org/0000-0002-3933-7677</orcidid><orcidid>https://orcid.org/0000-0002-3398-6916</orcidid><orcidid>https://orcid.org/0000-0002-2554-1837</orcidid><orcidid>https://orcid.org/0000-0002-1707-1775</orcidid><orcidid>https://orcid.org/0000-0003-3037-257X</orcidid><orcidid>https://orcid.org/0000-0003-4793-7880</orcidid><orcidid>https://orcid.org/0000-0002-0729-2988</orcidid><orcidid>https://orcid.org/0000-0001-7147-3575</orcidid><orcidid>https://orcid.org/0000-0003-2376-8971</orcidid><orcidid>https://orcid.org/0000-0003-1748-2010</orcidid><orcidid>https://orcid.org/0000-0001-6586-8845</orcidid><orcidid>https://orcid.org/0000-0003-4678-3939</orcidid><orcidid>https://orcid.org/0000-0003-2027-8221</orcidid><orcidid>https://orcid.org/0000-0001-5434-5942</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2018-05, Vol.859 (1), p.12 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_hal_02375607v1 |
| source | EZB Free E-Journals |
| subjects | Angular resolution Astrophysics Clumps Continuum radiation Cosmic dust Disks Dust Dust emission Emission Emitters Galaxies galaxies: evolution galaxies: ISM High resolution Interstellar matter Interstellar medium Morphology Red shift Sciences of the Universe Spectral emittance Star & galaxy formation Star formation Star formation rate Stars & galaxies submillimeter: galaxies Substructures |
| title | The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift |
| url | http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-09-21T14%3A58%3A31IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_hal_p&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20Dust%20and%20%5BC%20ii%5D%20Morphologies%20of%20Redshift%20%E2%88%BC4.5%20Sub-millimeter%20Galaxies%20at%20%E2%88%BC200%20pc%20Resolution:%20The%20Absence%20of%20Large%20Clumps%20in%20the%20Interstellar%20Medium%20at%20High-redshift&rft.jtitle=The%20Astrophysical%20journal&rft.au=Gullberg,%20B.&rft.date=2018-05-20&rft.volume=859&rft.issue=1&rft.spage=12&rft.pages=12-&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.3847/1538-4357/aabe8c&rft_dat=%3Cproquest_hal_p%3E2365927505%3C/proquest_hal_p%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c394c-e255fcdd36ba25b022da456c23fd28f753ea7f5e32a99804d2027df061e13bc73%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=2365927505&rft_id=info:pmid/&rfr_iscdi=true |