HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- II. The Local Void and its substructure
The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its sur...
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| creator | Kurapati, Sushma Kraan-Korteweg, Renée C Pisano, D J Chen, Hao Sambatriniaina H A Rajohnson Steyn, Nadia Bradley, Frank Serra, Paolo Goedhart, Sharmila Camilo, Fernando |
| description | The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329\(^{\circ}< \ell |
| doi_str_mv | 10.48550/arxiv.2312.05237 |
| format | Article |
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The Local Void and its substructure</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Kurapati, Sushma ; Kraan-Korteweg, Renée C ; Pisano, D J ; Chen, Hao ; Sambatriniaina H A Rajohnson ; Steyn, Nadia ; Bradley, Frank ; Serra, Paolo ; Goedhart, Sharmila ; Camilo, Fernando</creator><creatorcontrib>Kurapati, Sushma ; Kraan-Korteweg, Renée C ; Pisano, D J ; Chen, Hao ; Sambatriniaina H A Rajohnson ; Steyn, Nadia ; Bradley, Frank ; Serra, Paolo ; Goedhart, Sharmila ; Camilo, Fernando</creatorcontrib><description><![CDATA[The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329\(^{\circ}< \ell <\) 55\(^{\circ}\), Galactic latitude \(|b| <\) 1.5\(^{\circ}\), and redshift \(cz <\) 7500 km/s. We have detected 291 galaxies to median rms sensitivity of 0.44 mJy per beam per 44 km/s channel. We find 17 galaxies deep inside the Void, 96 at the border of the Void, while the remaining 178 galaxies are in average density environments. The extent of the Void is ~ 58 Mpc. It is severely under-dense for the longitude range 350\(^{\circ}< \ell <\) 35\(^{\circ}\) up to redshift \(z <\) 4500 km/s. The galaxies in the Void tend to have \HI masses that are lower (by approximately 0.25 dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void.]]></description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2312.05237</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Density ; Emission analysis ; Galactic bulge ; Galaxies ; Longitude ; Physics - Astrophysics of Galaxies ; Red shift</subject><ispartof>arXiv.org, 2023-12</ispartof><rights>2023. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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The Local Void and its substructure</title><title>arXiv.org</title><description><![CDATA[The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329\(^{\circ}< \ell <\) 55\(^{\circ}\), Galactic latitude \(|b| <\) 1.5\(^{\circ}\), and redshift \(cz <\) 7500 km/s. We have detected 291 galaxies to median rms sensitivity of 0.44 mJy per beam per 44 km/s channel. We find 17 galaxies deep inside the Void, 96 at the border of the Void, while the remaining 178 galaxies are in average density environments. The extent of the Void is ~ 58 Mpc. It is severely under-dense for the longitude range 350\(^{\circ}< \ell <\) 35\(^{\circ}\) up to redshift \(z <\) 4500 km/s. The galaxies in the Void tend to have \HI masses that are lower (by approximately 0.25 dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void.]]></description><subject>Density</subject><subject>Emission analysis</subject><subject>Galactic bulge</subject><subject>Galaxies</subject><subject>Longitude</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Red shift</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotkF1LwzAYhYMgOOZ-gFcGvG5N89Ekl2XoVpxMXPG2vG0T7ajtTNqx_ft1m1fn4jwcDg9CDxEJuRKCPIM71PuQsoiGRFAmb9CEMhYFilN6h2bebwkhNJZUCDZB22WKF9DA4Yg39XcL_eCMx3WL-x-DN8lnssbvxri3JLtgZV-X-KOBdiwHtzdHHAQ4TUOcjfiqK6HBX11dYWgrXPce-6HwvRvK8-w9urXQeDP7zynKXl-y-TJYrRfpPFkFIGgcKAmx0KyUVlXaWltQSZSm2paMRLrikkZKxjqWhVSloBwKxjkBxW1BwIBlU_R4nb2IyHeu_gV3zM9C8ouQkXi6EjvX_Q3G9_m2G1w7fsqpJoQzFauYnQCbY2DM</recordid><startdate>20231208</startdate><enddate>20231208</enddate><creator>Kurapati, Sushma</creator><creator>Kraan-Korteweg, Renée C</creator><creator>Pisano, D J</creator><creator>Chen, Hao</creator><creator>Sambatriniaina H A Rajohnson</creator><creator>Steyn, Nadia</creator><creator>Bradley, Frank</creator><creator>Serra, Paolo</creator><creator>Goedhart, Sharmila</creator><creator>Camilo, Fernando</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>20231208</creationdate><title>HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- II. 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It is severely under-dense for the longitude range 350\(^{\circ}< \ell <\) 35\(^{\circ}\) up to redshift \(z <\) 4500 km/s. The galaxies in the Void tend to have \HI masses that are lower (by approximately 0.25 dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void.]]></abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2312.05237</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Density Emission analysis Galactic bulge Galaxies Longitude Physics - Astrophysics of Galaxies Red shift |
| title | HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- II. The Local Void and its substructure |
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