The Four‐Quadrant Phase Mask Coronagraph. IV. First Light at the Very Large Telescope
We present the first high‐contrast images obtained at the ESO Very Large Telescope using a four‐quadrant phase mask coronagraph. The two‐night commissioning was carried out in 2004 January on NACO, the near‐IR camera with adaptive optics at UT4. We evaluated the behavior of the coronagraph on a vari...
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| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 2004-11, Vol.116 (825), p.1061-1071 |
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| container_title | Publications of the Astronomical Society of the Pacific |
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| creator | Boccaletti, A. Riaud, P. Baudoz, P. Baudrand, J. Rouan, D. Gratadour, D. Lacombe, F. Lagrange, A.‐M. |
| description | We present the first high‐contrast images obtained at the ESO Very Large Telescope using a four‐quadrant phase mask coronagraph. The two‐night commissioning was carried out in 2004 January on NACO, the near‐IR camera with adaptive optics at UT4. We evaluated the behavior of the coronagraph on a variety of astrophysical targets: binary stars, circumstellar disks, and active galactic nuclei. The performance of the coronagraph is in agreement with our expectations based on numerical simulations. The phase mask provides a stellar peak attenuation of a factor of about 10 on average (for long exposure), and its performance is limited only by the phase residuals (mainly low‐order aberrations) that are left uncorrected by the adaptive optics system. |
| doi_str_mv | 10.1086/425735 |
| format | Article |
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We evaluated the behavior of the coronagraph on a variety of astrophysical targets: binary stars, circumstellar disks, and active galactic nuclei. The performance of the coronagraph is in agreement with our expectations based on numerical simulations. The phase mask provides a stellar peak attenuation of a factor of about 10 on average (for long exposure), and its performance is limited only by the phase residuals (mainly low‐order aberrations) that are left uncorrected by the adaptive optics system.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>DOI: 10.1086/425735</identifier><identifier>CODEN: PASPAU</identifier><language>eng</language><publisher>Chicago, IL: The University of Chicago Press</publisher><subject>Angular separation ; Astronomical objects ; Astrophysics ; Coronagraphs ; Extrasolar planet detection ; Imaging ; Phase shift ; Physics ; Stars ; Telescopes ; Wave diffraction ; Wavelengths</subject><ispartof>Publications of the Astronomical Society of the Pacific, 2004-11, Vol.116 (825), p.1061-1071</ispartof><rights>2004. The Astronomical Society of the Pacific. All rights reserved. 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The phase mask provides a stellar peak attenuation of a factor of about 10 on average (for long exposure), and its performance is limited only by the phase residuals (mainly low‐order aberrations) that are left uncorrected by the adaptive optics system.</description><subject>Angular separation</subject><subject>Astronomical objects</subject><subject>Astrophysics</subject><subject>Coronagraphs</subject><subject>Extrasolar planet detection</subject><subject>Imaging</subject><subject>Phase shift</subject><subject>Physics</subject><subject>Stars</subject><subject>Telescopes</subject><subject>Wave diffraction</subject><subject>Wavelengths</subject><issn>0004-6280</issn><issn>1538-3873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2004</creationdate><recordtype>article</recordtype><recordid>eNp1kNFKwzAUhoMoOKc-Q0AUvOjMSdomvRzDuUFFhTkvy0mXrJ11HUkn7M5H8Bl9EjsqeuXVgZ_v_zj8hJwDGwBT8U3IIymiA9KDSKhAKCkOSY8xFgYxV-yYnHi_YgxAAeuRl1lh6Ljeuq-Pz6ctLhyuG_pYoDf0Hv0rHdWuXuPS4aYY0Ol8QMel8w1Ny2XRUGxo09bnxu1oim5p6MxUxuf1xpySI4uVN2c_t0-ex7ez0SRIH-6mo2Ea5EJBE1hpw1DohbJKRoJLwUNhOSQJMi4TqcNIGoaw0AoUaqm14VzENgHLdawjLfrkuvMWWGUbV76h22U1ltlkmGb7jAnFoHW_Q8tedWzuau-dsb8FYNl-uqybrgUvO3CDPsfKtqPkpf-jYwEQtn_3yUXHrXxTu_9s39T1dkE</recordid><startdate>20041101</startdate><enddate>20041101</enddate><creator>Boccaletti, A.</creator><creator>Riaud, P.</creator><creator>Baudoz, P.</creator><creator>Baudrand, J.</creator><creator>Rouan, D.</creator><creator>Gratadour, D.</creator><creator>Lacombe, F.</creator><creator>Lagrange, A.‐M.</creator><general>The University of Chicago Press</general><general>University of Chicago Press</general><general>Astronomical Society of the Pacific</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><orcidid>https://orcid.org/0000-0003-2080-7189</orcidid></search><sort><creationdate>20041101</creationdate><title>The Four‐Quadrant Phase Mask Coronagraph. 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First Light at the Very Large Telescope</title><author>Boccaletti, A. ; Riaud, P. ; Baudoz, P. ; Baudrand, J. ; Rouan, D. ; Gratadour, D. ; Lacombe, F. ; Lagrange, A.‐M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c381t-f7f443bd8f8753273243f2199a02797b457e0a1db818ab7bbe2236f91f2b6b5b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2004</creationdate><topic>Angular separation</topic><topic>Astronomical objects</topic><topic>Astrophysics</topic><topic>Coronagraphs</topic><topic>Extrasolar planet detection</topic><topic>Imaging</topic><topic>Phase shift</topic><topic>Physics</topic><topic>Stars</topic><topic>Telescopes</topic><topic>Wave diffraction</topic><topic>Wavelengths</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Boccaletti, A.</creatorcontrib><creatorcontrib>Riaud, P.</creatorcontrib><creatorcontrib>Baudoz, P.</creatorcontrib><creatorcontrib>Baudrand, J.</creatorcontrib><creatorcontrib>Rouan, D.</creatorcontrib><creatorcontrib>Gratadour, D.</creatorcontrib><creatorcontrib>Lacombe, F.</creatorcontrib><creatorcontrib>Lagrange, A.‐M.</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Publications of the Astronomical Society of the Pacific</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Boccaletti, A.</au><au>Riaud, P.</au><au>Baudoz, P.</au><au>Baudrand, J.</au><au>Rouan, D.</au><au>Gratadour, D.</au><au>Lacombe, F.</au><au>Lagrange, A.‐M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Four‐Quadrant Phase Mask Coronagraph. IV. First Light at the Very Large Telescope</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>2004-11-01</date><risdate>2004</risdate><volume>116</volume><issue>825</issue><spage>1061</spage><epage>1071</epage><pages>1061-1071</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><coden>PASPAU</coden><abstract>We present the first high‐contrast images obtained at the ESO Very Large Telescope using a four‐quadrant phase mask coronagraph. The two‐night commissioning was carried out in 2004 January on NACO, the near‐IR camera with adaptive optics at UT4. We evaluated the behavior of the coronagraph on a variety of astrophysical targets: binary stars, circumstellar disks, and active galactic nuclei. The performance of the coronagraph is in agreement with our expectations based on numerical simulations. 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| issn | 0004-6280 1538-3873 |
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| source | IOP Publishing Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; JSTOR Archive Collection A-Z Listing; Institute of Physics (IOP) Journals - HEAL-Link; Alma/SFX Local Collection |
| subjects | Angular separation Astronomical objects Astrophysics Coronagraphs Extrasolar planet detection Imaging Phase shift Physics Stars Telescopes Wave diffraction Wavelengths |
| title | The Four‐Quadrant Phase Mask Coronagraph. IV. First Light at the Very Large Telescope |
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