Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13
We have carried out an intensive study of photometric (Kepler Mission) and spectroscopic data on the system Kepler -2 (HAT-P-7A) using the dedicated software WinFitter 6.4 . The mean individual data-point error of the normalized flux values for this system is 0.00015, leading to the model’s specific...
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| description | We have carried out an intensive study of photometric (Kepler Mission) and spectroscopic data on the system
Kepler
-2 (HAT-P-7A) using the dedicated software
WinFitter 6.4
. The mean individual data-point error of the normalized flux values for this system is 0.00015, leading to the model’s specification for the mean reference flux to an accuracy of ∼0.5 ppm. This testifies to the remarkably high accuracy of the binned data-set, derived from over 1.8 million individual observations. Spectroscopic data are reported with the similarly high-accuracy radial velocity amplitude measure of ∼2 m s
−1
. The analysis includes discussion of the fitting quality and model adequacy.
Our derived absolute parameters for
Kepler
-2 are as follows:
M
p
(Jupiter) 1.80 ± 0.13;
R
⋆
1.46
±
0.08
×
10
6
km;
R
p
1.15
±
0.07
×
10
5
km. These values imply somewhat larger and less condensed bodies than previously catalogued, but within reasonable error estimates of such literature parameters.
We find also tidal, reflection and Doppler effect parameters, showing that the optimal model specification differs slightly from a ‘cleaned’ model that reduces the standard deviation of the ∼3600 binned light curve points to less than 0.9 ppm. We consider these slight differences, making comparisons with the hot-Jupiter systems
Kepler
-1 (TrES-2) and 13.
We confirm that the star’s rotation axis must be shifted towards the line of sight, though how closely depends on what rotation velocity is adopted for the star. From joint analysis of the spectroscopic and photometric data we find an equatorial rotation speed of 11 ± 3 km s
−1
.
A slightly brighter region of the photosphere that distorts the transit shape can be interpreted as an indication of the gravity effect at the rotation pole; however we note that the geometry for this does not match the spectroscopic result. We discuss this difference, rejecting the possibility that a real shift in the position of the rotation axis in the few years between the spectroscopic and photometric data-collection times. Alternative explanations are considered, but we conclude that renewed detailed observations are required to help settle these questions. |
| doi_str_mv | 10.1007/s10509-020-03789-3 |
| format | Article |
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Kepler
-2 (HAT-P-7A) using the dedicated software
WinFitter 6.4
. The mean individual data-point error of the normalized flux values for this system is 0.00015, leading to the model’s specification for the mean reference flux to an accuracy of ∼0.5 ppm. This testifies to the remarkably high accuracy of the binned data-set, derived from over 1.8 million individual observations. Spectroscopic data are reported with the similarly high-accuracy radial velocity amplitude measure of ∼2 m s
−1
. The analysis includes discussion of the fitting quality and model adequacy.
Our derived absolute parameters for
Kepler
-2 are as follows:
M
p
(Jupiter) 1.80 ± 0.13;
R
⋆
1.46
±
0.08
×
10
6
km;
R
p
1.15
±
0.07
×
10
5
km. These values imply somewhat larger and less condensed bodies than previously catalogued, but within reasonable error estimates of such literature parameters.
We find also tidal, reflection and Doppler effect parameters, showing that the optimal model specification differs slightly from a ‘cleaned’ model that reduces the standard deviation of the ∼3600 binned light curve points to less than 0.9 ppm. We consider these slight differences, making comparisons with the hot-Jupiter systems
Kepler
-1 (TrES-2) and 13.
We confirm that the star’s rotation axis must be shifted towards the line of sight, though how closely depends on what rotation velocity is adopted for the star. From joint analysis of the spectroscopic and photometric data we find an equatorial rotation speed of 11 ± 3 km s
−1
.
A slightly brighter region of the photosphere that distorts the transit shape can be interpreted as an indication of the gravity effect at the rotation pole; however we note that the geometry for this does not match the spectroscopic result. We discuss this difference, rejecting the possibility that a real shift in the position of the rotation axis in the few years between the spectroscopic and photometric data-collection times. Alternative explanations are considered, but we conclude that renewed detailed observations are required to help settle these questions.</description><identifier>ISSN: 0004-640X</identifier><identifier>EISSN: 1572-946X</identifier><identifier>DOI: 10.1007/s10509-020-03789-3</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Accuracy ; Adequacy ; Astrobiology ; Astronomy ; Astrophysics ; Astrophysics and Astroparticles ; Cosmology ; Data collection ; Doppler effect ; Extrasolar planets ; Gravity effects ; Jupiter ; Kepler mission (NASA) ; Light curve ; Mathematical models ; Observations and Techniques ; Original Article ; Parameter estimation ; Photometry ; Photosphere ; Physics ; Physics and Astronomy ; Radial velocity ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Specifications ; Stellar rotation</subject><ispartof>Astrophysics and space science, 2020-04, Vol.365 (4), Article 77</ispartof><rights>Springer Nature B.V. 2020</rights><rights>Springer Nature B.V. 2020.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c270t-48ccd097d0159abce1a22770c9c3247065de6ad727c7f4c7a6004ce5247d09093</cites><orcidid>0000-0001-9445-4588</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s10509-020-03789-3$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s10509-020-03789-3$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Rhodes, Michael D.</creatorcontrib><creatorcontrib>Püsküllü, Çağlar</creatorcontrib><creatorcontrib>Budding, Edwin</creatorcontrib><creatorcontrib>Banks, Timothy S.</creatorcontrib><title>Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13</title><title>Astrophysics and space science</title><addtitle>Astrophys Space Sci</addtitle><description>We have carried out an intensive study of photometric (Kepler Mission) and spectroscopic data on the system
Kepler
-2 (HAT-P-7A) using the dedicated software
WinFitter 6.4
. The mean individual data-point error of the normalized flux values for this system is 0.00015, leading to the model’s specification for the mean reference flux to an accuracy of ∼0.5 ppm. This testifies to the remarkably high accuracy of the binned data-set, derived from over 1.8 million individual observations. Spectroscopic data are reported with the similarly high-accuracy radial velocity amplitude measure of ∼2 m s
−1
. The analysis includes discussion of the fitting quality and model adequacy.
Our derived absolute parameters for
Kepler
-2 are as follows:
M
p
(Jupiter) 1.80 ± 0.13;
R
⋆
1.46
±
0.08
×
10
6
km;
R
p
1.15
±
0.07
×
10
5
km. These values imply somewhat larger and less condensed bodies than previously catalogued, but within reasonable error estimates of such literature parameters.
We find also tidal, reflection and Doppler effect parameters, showing that the optimal model specification differs slightly from a ‘cleaned’ model that reduces the standard deviation of the ∼3600 binned light curve points to less than 0.9 ppm. We consider these slight differences, making comparisons with the hot-Jupiter systems
Kepler
-1 (TrES-2) and 13.
We confirm that the star’s rotation axis must be shifted towards the line of sight, though how closely depends on what rotation velocity is adopted for the star. From joint analysis of the spectroscopic and photometric data we find an equatorial rotation speed of 11 ± 3 km s
−1
.
A slightly brighter region of the photosphere that distorts the transit shape can be interpreted as an indication of the gravity effect at the rotation pole; however we note that the geometry for this does not match the spectroscopic result. We discuss this difference, rejecting the possibility that a real shift in the position of the rotation axis in the few years between the spectroscopic and photometric data-collection times. Alternative explanations are considered, but we conclude that renewed detailed observations are required to help settle these questions.</description><subject>Accuracy</subject><subject>Adequacy</subject><subject>Astrobiology</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Cosmology</subject><subject>Data collection</subject><subject>Doppler effect</subject><subject>Extrasolar planets</subject><subject>Gravity effects</subject><subject>Jupiter</subject><subject>Kepler mission (NASA)</subject><subject>Light curve</subject><subject>Mathematical models</subject><subject>Observations and Techniques</subject><subject>Original Article</subject><subject>Parameter estimation</subject><subject>Photometry</subject><subject>Photosphere</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Radial velocity</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Specifications</subject><subject>Stellar rotation</subject><issn>0004-640X</issn><issn>1572-946X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNp9kEFLAzEQhYMoWKt_wFPAc3SS7GY2Bw9SahULXhR6CzGbast2syZbtP_e1FW8eRqGee_NzEfIOYdLDoBXiUMJmoEABhIrzeQBGfESBdOFWhySEQAUTBWwOCYnKa1zq5XGEbmefoausa3vadql3m_og-8aH5mgH6v-jbqw6WxcpdAm2offIae2rSmXp-RoaZvkz37qmDzfTp8md2z-OLuf3MyZEwg9KyrnatBYAy-1fXGeWyEQwWknRYGgytorW6NAh8vCoVX5WufLPMs20HJMLobcLob3rU-9WYdtbPNKI6RW-U-o9ioxqFwMKUW_NF1cbWzcGQ5mj8kMmEzGZL4xGZlNcjClLG5fffyL_sf1BTk_aIo</recordid><startdate>20200401</startdate><enddate>20200401</enddate><creator>Rhodes, Michael D.</creator><creator>Püsküllü, Çağlar</creator><creator>Budding, Edwin</creator><creator>Banks, Timothy S.</creator><general>Springer Netherlands</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AEUYN</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope><orcidid>https://orcid.org/0000-0001-9445-4588</orcidid></search><sort><creationdate>20200401</creationdate><title>Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13</title><author>Rhodes, Michael D. ; Püsküllü, Çağlar ; Budding, Edwin ; Banks, Timothy S.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c270t-48ccd097d0159abce1a22770c9c3247065de6ad727c7f4c7a6004ce5247d09093</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Accuracy</topic><topic>Adequacy</topic><topic>Astrobiology</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Astrophysics and Astroparticles</topic><topic>Cosmology</topic><topic>Data collection</topic><topic>Doppler effect</topic><topic>Extrasolar planets</topic><topic>Gravity effects</topic><topic>Jupiter</topic><topic>Kepler mission (NASA)</topic><topic>Light curve</topic><topic>Mathematical models</topic><topic>Observations and Techniques</topic><topic>Original Article</topic><topic>Parameter estimation</topic><topic>Photometry</topic><topic>Photosphere</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Radial velocity</topic><topic>Space Exploration and Astronautics</topic><topic>Space Sciences (including Extraterrestrial Physics</topic><topic>Specifications</topic><topic>Stellar rotation</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Rhodes, Michael D.</creatorcontrib><creatorcontrib>Püsküllü, Çağlar</creatorcontrib><creatorcontrib>Budding, Edwin</creatorcontrib><creatorcontrib>Banks, Timothy S.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</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>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</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 Basic</collection><jtitle>Astrophysics and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Rhodes, Michael D.</au><au>Püsküllü, Çağlar</au><au>Budding, Edwin</au><au>Banks, Timothy S.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13</atitle><jtitle>Astrophysics and space science</jtitle><stitle>Astrophys Space Sci</stitle><date>2020-04-01</date><risdate>2020</risdate><volume>365</volume><issue>4</issue><artnum>77</artnum><issn>0004-640X</issn><eissn>1572-946X</eissn><abstract>We have carried out an intensive study of photometric (Kepler Mission) and spectroscopic data on the system
Kepler
-2 (HAT-P-7A) using the dedicated software
WinFitter 6.4
. The mean individual data-point error of the normalized flux values for this system is 0.00015, leading to the model’s specification for the mean reference flux to an accuracy of ∼0.5 ppm. This testifies to the remarkably high accuracy of the binned data-set, derived from over 1.8 million individual observations. Spectroscopic data are reported with the similarly high-accuracy radial velocity amplitude measure of ∼2 m s
−1
. The analysis includes discussion of the fitting quality and model adequacy.
Our derived absolute parameters for
Kepler
-2 are as follows:
M
p
(Jupiter) 1.80 ± 0.13;
R
⋆
1.46
±
0.08
×
10
6
km;
R
p
1.15
±
0.07
×
10
5
km. These values imply somewhat larger and less condensed bodies than previously catalogued, but within reasonable error estimates of such literature parameters.
We find also tidal, reflection and Doppler effect parameters, showing that the optimal model specification differs slightly from a ‘cleaned’ model that reduces the standard deviation of the ∼3600 binned light curve points to less than 0.9 ppm. We consider these slight differences, making comparisons with the hot-Jupiter systems
Kepler
-1 (TrES-2) and 13.
We confirm that the star’s rotation axis must be shifted towards the line of sight, though how closely depends on what rotation velocity is adopted for the star. From joint analysis of the spectroscopic and photometric data we find an equatorial rotation speed of 11 ± 3 km s
−1
.
A slightly brighter region of the photosphere that distorts the transit shape can be interpreted as an indication of the gravity effect at the rotation pole; however we note that the geometry for this does not match the spectroscopic result. We discuss this difference, rejecting the possibility that a real shift in the position of the rotation axis in the few years between the spectroscopic and photometric data-collection times. Alternative explanations are considered, but we conclude that renewed detailed observations are required to help settle these questions.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s10509-020-03789-3</doi><orcidid>https://orcid.org/0000-0001-9445-4588</orcidid></addata></record> |
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| source | SpringerLink Journals - AutoHoldings |
| subjects | Accuracy Adequacy Astrobiology Astronomy Astrophysics Astrophysics and Astroparticles Cosmology Data collection Doppler effect Extrasolar planets Gravity effects Jupiter Kepler mission (NASA) Light curve Mathematical models Observations and Techniques Original Article Parameter estimation Photometry Photosphere Physics Physics and Astronomy Radial velocity Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Specifications Stellar rotation |
| title | Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13 |
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