Phase-Referenced VLBA Observations of OH Masers at 4765 MHz
Astrophys.J.599:324-334,2003 We report VLBA observations of maser emission from the rotationally excited doublet Pi 1/2, J=1/2 state of OH at 4765 MHz. We made phase-referenced observations of W3(OH) at both 4765 MHz and 1720 MHz and found emission in three fields within a about 2000 AU diameter reg...
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| creator | Palmer, Patrick Goss, W. M Devine, K. E |
| description | Astrophys.J.599:324-334,2003 We report VLBA observations of maser emission from the rotationally excited
doublet Pi 1/2, J=1/2 state of OH at 4765 MHz. We made phase-referenced
observations of W3(OH) at both 4765 MHz and 1720 MHz and found emission in
three fields within a about 2000 AU diameter region and verified that in two of
the three fields, 4765 MHz and 1720 MHz emission arise from the same position
to within about 4 mas (about 5 AU diameter emission regions along an
approximately N-S arc with linear extent about 500 AU. In addition, we carried
out phase-referenced observations of 4765 MHz emission from K3-50. We searched
for the 4765 MHz line in W49 (without phase referencing) and W75N
(phase-referenced to the strongest 4765 MHz maser feature in DR21EX); we were
unable to detect these sources with the VLBA. For 2 1/2 years (including the
dates of the VLBA observations), we carried out monitoring observations of 4765
MHz emission with the VLA. Constraints on models for maser emission at 1720 MHz
and 4765 MHz are derived from the observations. These observations are then
briefly compared with existing models. |
| doi_str_mv | 10.48550/arxiv.astro-ph/0309078 |
| format | Article |
| fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_astro_ph_0309078</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>astro_ph_0309078</sourcerecordid><originalsourceid>FETCH-arxiv_primary_astro_ph_03090783</originalsourceid><addsrcrecordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNA3MDawNDC34GSwDshILE7VDUpNSy1KzUtOTVEI83FyVPBPKk4tKkssyczPK1bIT1Pw91DwBaorKlZILFEwMTczVfD1qOJhYE1LzClO5YXS3Ayqbq4hzh66YMviC4oycxOLKuPBlsYXZMRDLTUmVh0ArIE7Zw</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Phase-Referenced VLBA Observations of OH Masers at 4765 MHz</title><source>arXiv.org</source><creator>Palmer, Patrick ; Goss, W. M ; Devine, K. E</creator><creatorcontrib>Palmer, Patrick ; Goss, W. M ; Devine, K. E</creatorcontrib><description>Astrophys.J.599:324-334,2003 We report VLBA observations of maser emission from the rotationally excited
doublet Pi 1/2, J=1/2 state of OH at 4765 MHz. We made phase-referenced
observations of W3(OH) at both 4765 MHz and 1720 MHz and found emission in
three fields within a about 2000 AU diameter region and verified that in two of
the three fields, 4765 MHz and 1720 MHz emission arise from the same position
to within about 4 mas (about 5 AU diameter emission regions along an
approximately N-S arc with linear extent about 500 AU. In addition, we carried
out phase-referenced observations of 4765 MHz emission from K3-50. We searched
for the 4765 MHz line in W49 (without phase referencing) and W75N
(phase-referenced to the strongest 4765 MHz maser feature in DR21EX); we were
unable to detect these sources with the VLBA. For 2 1/2 years (including the
dates of the VLBA observations), we carried out monitoring observations of 4765
MHz emission with the VLA. Constraints on models for maser emission at 1720 MHz
and 4765 MHz are derived from the observations. These observations are then
briefly compared with existing models.</description><identifier>DOI: 10.48550/arxiv.astro-ph/0309078</identifier><language>eng</language><subject>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</subject><creationdate>2003-09</creationdate><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,881</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/astro-ph/0309078$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.astro-ph/0309078$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1086/379195$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Palmer, Patrick</creatorcontrib><creatorcontrib>Goss, W. M</creatorcontrib><creatorcontrib>Devine, K. E</creatorcontrib><title>Phase-Referenced VLBA Observations of OH Masers at 4765 MHz</title><description>Astrophys.J.599:324-334,2003 We report VLBA observations of maser emission from the rotationally excited
doublet Pi 1/2, J=1/2 state of OH at 4765 MHz. We made phase-referenced
observations of W3(OH) at both 4765 MHz and 1720 MHz and found emission in
three fields within a about 2000 AU diameter region and verified that in two of
the three fields, 4765 MHz and 1720 MHz emission arise from the same position
to within about 4 mas (about 5 AU diameter emission regions along an
approximately N-S arc with linear extent about 500 AU. In addition, we carried
out phase-referenced observations of 4765 MHz emission from K3-50. We searched
for the 4765 MHz line in W49 (without phase referencing) and W75N
(phase-referenced to the strongest 4765 MHz maser feature in DR21EX); we were
unable to detect these sources with the VLBA. For 2 1/2 years (including the
dates of the VLBA observations), we carried out monitoring observations of 4765
MHz emission with the VLA. Constraints on models for maser emission at 1720 MHz
and 4765 MHz are derived from the observations. These observations are then
briefly compared with existing models.</description><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><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2003</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNA3MDawNDC34GSwDshILE7VDUpNSy1KzUtOTVEI83FyVPBPKk4tKkssyczPK1bIT1Pw91DwBaorKlZILFEwMTczVfD1qOJhYE1LzClO5YXS3Ayqbq4hzh66YMviC4oycxOLKuPBlsYXZMRDLTUmVh0ArIE7Zw</recordid><startdate>20030902</startdate><enddate>20030902</enddate><creator>Palmer, Patrick</creator><creator>Goss, W. M</creator><creator>Devine, K. E</creator><scope>GOX</scope></search><sort><creationdate>20030902</creationdate><title>Phase-Referenced VLBA Observations of OH Masers at 4765 MHz</title><author>Palmer, Patrick ; Goss, W. M ; Devine, K. E</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_astro_ph_03090783</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2003</creationdate><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><toplevel>online_resources</toplevel><creatorcontrib>Palmer, Patrick</creatorcontrib><creatorcontrib>Goss, W. M</creatorcontrib><creatorcontrib>Devine, K. E</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Palmer, Patrick</au><au>Goss, W. M</au><au>Devine, K. E</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Phase-Referenced VLBA Observations of OH Masers at 4765 MHz</atitle><date>2003-09-02</date><risdate>2003</risdate><abstract>Astrophys.J.599:324-334,2003 We report VLBA observations of maser emission from the rotationally excited
doublet Pi 1/2, J=1/2 state of OH at 4765 MHz. We made phase-referenced
observations of W3(OH) at both 4765 MHz and 1720 MHz and found emission in
three fields within a about 2000 AU diameter region and verified that in two of
the three fields, 4765 MHz and 1720 MHz emission arise from the same position
to within about 4 mas (about 5 AU diameter emission regions along an
approximately N-S arc with linear extent about 500 AU. In addition, we carried
out phase-referenced observations of 4765 MHz emission from K3-50. We searched
for the 4765 MHz line in W49 (without phase referencing) and W75N
(phase-referenced to the strongest 4765 MHz maser feature in DR21EX); we were
unable to detect these sources with the VLBA. For 2 1/2 years (including the
dates of the VLBA observations), we carried out monitoring observations of 4765
MHz emission with the VLA. Constraints on models for maser emission at 1720 MHz
and 4765 MHz are derived from the observations. These observations are then
briefly compared with existing models.</abstract><doi>10.48550/arxiv.astro-ph/0309078</doi><oa>free_for_read</oa></addata></record> |
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| subjects | 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 |
| title | Phase-Referenced VLBA Observations of OH Masers at 4765 MHz |
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