A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi
Dust permeates the interstellar medium, reddening and polarizing background starlight, but dust properties vary with local environment. In order to characterize dust in a highly irradiated diffuse cloud, we measure the reddening and optical polarization towards 27 stars surrounding the mid-latitude...
Gespeichert in:
| Veröffentlicht in: | arXiv.org 2021-12 |
|---|---|
| Hauptverfasser: | , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | |
| container_start_page | |
| container_title | arXiv.org |
| container_volume | |
| creator | Piccone, Ashley N Kobulnicky, Chip |
| description | Dust permeates the interstellar medium, reddening and polarizing background starlight, but dust properties vary with local environment. In order to characterize dust in a highly irradiated diffuse cloud, we measure the reddening and optical polarization towards 27 stars surrounding the mid-latitude \(b\)=\(+\)24\(^{\circ}\) O9.2IV star \(\zeta\) Ophiuchi, using new optical spectroscopy and polarimetry. We incrementally deredden and depolarize with distance, allowing us to distinguish dust components along these sightlines. The data indicate three distinct dust populations: a foreground component characteristic of average Milky Way dust ($R_{\rm{V}}$$\approx\(3.1, \)d$$\lesssim\(180 pc), a highly polarizing mid-distance component in the vicinity of \)\zeta\( Oph (\)R_{\rm{V}}$$\approx\(2.4, 200 pc\) |
| doi_str_mv | 10.48550/arxiv.2112.12214 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest</sourceid><recordid>TN_cdi_proquest_journals_2613417358</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2613417358</sourcerecordid><originalsourceid>FETCH-proquest_journals_26134173583</originalsourceid><addsrcrecordid>eNqNy81KAzEYheEgCBbtBbj7wI0uOiZfJu3grmjFnaJDVwNDtGknJU3G_GhpmXs3iBfg6izO-xByyWhRVkLQW-n3-qtAxrBgiKw8ISPknE2qEvGMjEPYUkpxOkMh-IgMc6ilUeDWUHdeKXhIIcKL65ORUTsb7mApvZbvuWmuX9tj43fH5TA0NyDtChb76NVOZWBydfglMDfObuBNb7potFUBavct_Sr75qCizPS573T66PQFOV1LE9T4b8_J1eOivn-a9N59JhViu3XJ23y1OGW8ZDMuKv6_6geLolSZ</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2613417358</pqid></control><display><type>article</type><title>A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi</title><source>Free E- Journals</source><creator>Piccone, Ashley N ; Kobulnicky, Chip</creator><creatorcontrib>Piccone, Ashley N ; Kobulnicky, Chip</creatorcontrib><description>Dust permeates the interstellar medium, reddening and polarizing background starlight, but dust properties vary with local environment. In order to characterize dust in a highly irradiated diffuse cloud, we measure the reddening and optical polarization towards 27 stars surrounding the mid-latitude \(b\)=\(+\)24\(^{\circ}\) O9.2IV star \(\zeta\) Ophiuchi, using new optical spectroscopy and polarimetry. We incrementally deredden and depolarize with distance, allowing us to distinguish dust components along these sightlines. The data indicate three distinct dust populations: a foreground component characteristic of average Milky Way dust ($R_{\rm{V}}$$\approx\(3.1, \)d$$\lesssim\(180 pc), a highly polarizing mid-distance component in the vicinity of \)\zeta\( Oph (\)R_{\rm{V}}$$\approx\(2.4, 200 pc\)<$$d$$<\(300 pc), and a non-polarizing distant component (\)R_{\rm{V}}$$\approx\(3.6, 600 pc\)<$$d$$<\(2000 pc). Prominent 8 \)\mu\(m infrared striations spanning the field of view likely have high Polycyclic Aromatic Hydrocarbon content and are illuminated by \)\zeta\( Oph. Foreground-subtracted polarizations roughly align with these striations, which, we argue, lie immediately behind \)\zeta\( Oph and constitute the highly-polarizing mid-distance dust. This component polarizes very efficiently (\)P_{\rm{V}}$$>\(9.1\)E(B-V)\(), implying a high degree of grain alignment and suggesting that the bulk of the polarization occurs in a small fraction of the volume. The large \)R_{\rm{V}}\( in the distant component reveals that dust above the Galactic Plane (\)z$$>$250 pc) may contain a greater fraction of large grains than the Milky Way average.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2112.12214</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Aromatic hydrocarbons ; Cosmic dust ; Depolarization ; Dust ; Field of view ; Interstellar matter ; Optical polarization ; Populations ; Striations</subject><ispartof>arXiv.org, 2021-12</ispartof><rights>2021. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>780,784,27925</link.rule.ids></links><search><creatorcontrib>Piccone, Ashley N</creatorcontrib><creatorcontrib>Kobulnicky, Chip</creatorcontrib><title>A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi</title><title>arXiv.org</title><description>Dust permeates the interstellar medium, reddening and polarizing background starlight, but dust properties vary with local environment. In order to characterize dust in a highly irradiated diffuse cloud, we measure the reddening and optical polarization towards 27 stars surrounding the mid-latitude \(b\)=\(+\)24\(^{\circ}\) O9.2IV star \(\zeta\) Ophiuchi, using new optical spectroscopy and polarimetry. We incrementally deredden and depolarize with distance, allowing us to distinguish dust components along these sightlines. The data indicate three distinct dust populations: a foreground component characteristic of average Milky Way dust ($R_{\rm{V}}$$\approx\(3.1, \)d$$\lesssim\(180 pc), a highly polarizing mid-distance component in the vicinity of \)\zeta\( Oph (\)R_{\rm{V}}$$\approx\(2.4, 200 pc\)<$$d$$<\(300 pc), and a non-polarizing distant component (\)R_{\rm{V}}$$\approx\(3.6, 600 pc\)<$$d$$<\(2000 pc). Prominent 8 \)\mu\(m infrared striations spanning the field of view likely have high Polycyclic Aromatic Hydrocarbon content and are illuminated by \)\zeta\( Oph. Foreground-subtracted polarizations roughly align with these striations, which, we argue, lie immediately behind \)\zeta\( Oph and constitute the highly-polarizing mid-distance dust. This component polarizes very efficiently (\)P_{\rm{V}}$$>\(9.1\)E(B-V)\(), implying a high degree of grain alignment and suggesting that the bulk of the polarization occurs in a small fraction of the volume. The large \)R_{\rm{V}}\( in the distant component reveals that dust above the Galactic Plane (\)z$$>$250 pc) may contain a greater fraction of large grains than the Milky Way average.</description><subject>Aromatic hydrocarbons</subject><subject>Cosmic dust</subject><subject>Depolarization</subject><subject>Dust</subject><subject>Field of view</subject><subject>Interstellar matter</subject><subject>Optical polarization</subject><subject>Populations</subject><subject>Striations</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><recordid>eNqNy81KAzEYheEgCBbtBbj7wI0uOiZfJu3grmjFnaJDVwNDtGknJU3G_GhpmXs3iBfg6izO-xByyWhRVkLQW-n3-qtAxrBgiKw8ISPknE2qEvGMjEPYUkpxOkMh-IgMc6ilUeDWUHdeKXhIIcKL65ORUTsb7mApvZbvuWmuX9tj43fH5TA0NyDtChb76NVOZWBydfglMDfObuBNb7potFUBavct_Sr75qCizPS573T66PQFOV1LE9T4b8_J1eOivn-a9N59JhViu3XJ23y1OGW8ZDMuKv6_6geLolSZ</recordid><startdate>20211222</startdate><enddate>20211222</enddate><creator>Piccone, Ashley N</creator><creator>Kobulnicky, Chip</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></search><sort><creationdate>20211222</creationdate><title>A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi</title><author>Piccone, Ashley N ; Kobulnicky, Chip</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-proquest_journals_26134173583</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Aromatic hydrocarbons</topic><topic>Cosmic dust</topic><topic>Depolarization</topic><topic>Dust</topic><topic>Field of view</topic><topic>Interstellar matter</topic><topic>Optical polarization</topic><topic>Populations</topic><topic>Striations</topic><toplevel>online_resources</toplevel><creatorcontrib>Piccone, Ashley N</creatorcontrib><creatorcontrib>Kobulnicky, Chip</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></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Piccone, Ashley N</au><au>Kobulnicky, Chip</au><format>book</format><genre>document</genre><ristype>GEN</ristype><atitle>A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi</atitle><jtitle>arXiv.org</jtitle><date>2021-12-22</date><risdate>2021</risdate><eissn>2331-8422</eissn><abstract>Dust permeates the interstellar medium, reddening and polarizing background starlight, but dust properties vary with local environment. In order to characterize dust in a highly irradiated diffuse cloud, we measure the reddening and optical polarization towards 27 stars surrounding the mid-latitude \(b\)=\(+\)24\(^{\circ}\) O9.2IV star \(\zeta\) Ophiuchi, using new optical spectroscopy and polarimetry. We incrementally deredden and depolarize with distance, allowing us to distinguish dust components along these sightlines. The data indicate three distinct dust populations: a foreground component characteristic of average Milky Way dust ($R_{\rm{V}}$$\approx\(3.1, \)d$$\lesssim\(180 pc), a highly polarizing mid-distance component in the vicinity of \)\zeta\( Oph (\)R_{\rm{V}}$$\approx\(2.4, 200 pc\)<$$d$$<\(300 pc), and a non-polarizing distant component (\)R_{\rm{V}}$$\approx\(3.6, 600 pc\)<$$d$$<\(2000 pc). Prominent 8 \)\mu\(m infrared striations spanning the field of view likely have high Polycyclic Aromatic Hydrocarbon content and are illuminated by \)\zeta\( Oph. Foreground-subtracted polarizations roughly align with these striations, which, we argue, lie immediately behind \)\zeta\( Oph and constitute the highly-polarizing mid-distance dust. This component polarizes very efficiently (\)P_{\rm{V}}$$>\(9.1\)E(B-V)\(), implying a high degree of grain alignment and suggesting that the bulk of the polarization occurs in a small fraction of the volume. The large \)R_{\rm{V}}\( in the distant component reveals that dust above the Galactic Plane (\)z$$>$250 pc) may contain a greater fraction of large grains than the Milky Way average.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2112.12214</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2021-12 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_proquest_journals_2613417358 |
| source | Free E- Journals |
| subjects | Aromatic hydrocarbons Cosmic dust Depolarization Dust Field of view Interstellar matter Optical polarization Populations Striations |
| title | A Tale of Three Dust Populations: Variable \(R_{\rm{V}}\) and Extreme Polarization Along Sightlines Toward \(\zeta\) Ophiuchi |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-27T10%3A15%3A48IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest&rft_val_fmt=info:ofi/fmt:kev:mtx:book&rft.genre=document&rft.atitle=A%20Tale%20of%20Three%20Dust%20Populations:%20Variable%20%5C(R_%7B%5Crm%7BV%7D%7D%5C)%20and%20Extreme%20Polarization%20Along%20Sightlines%20Toward%20%5C(%5Czeta%5C)%20Ophiuchi&rft.jtitle=arXiv.org&rft.au=Piccone,%20Ashley%20N&rft.date=2021-12-22&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2112.12214&rft_dat=%3Cproquest%3E2613417358%3C/proquest%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2613417358&rft_id=info:pmid/&rfr_iscdi=true |