TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
We report the discovery of a close-in ( P orb = 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby ( d = 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-i...
Gespeichert in:
| Veröffentlicht in: | The Astronomical journal 2024-08, Vol.168 (2), p.93 |
|---|---|
| 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 | 2 |
| container_start_page | 93 |
| container_title | The Astronomical journal |
| container_volume | 168 |
| creator | Jones, Sinclaire E. Stefánsson, Guđmundur Masuda, Kento Libby-Roberts, Jessica E. Gardner, Cristilyn N. Holcomb, Rae Beard, Corey Robertson, Paul Cañas, Caleb I. Mahadevan, Suvrath Kanodia, Shubham Lin, Andrea S. J. Kobulnicky, Henry A. Parker, Brock A. Bender, Chad F. Cochran, William D. Diddams, Scott A. Fernandes, Rachel B. Gupta, Arvind F. Halverson, Samuel Hawley, Suzanne L. Hearty, Fred R. Hebb, Leslie Kowalski, Adam Lubin, Jack Monson, Andrew Ninan, Joe P. Ramsey, Lawrence Roy, Arpita Schwab, Christian Terrien, Ryan C. Wisniewski, John |
| description | We report the discovery of a close-in (
P
orb
= 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby (
d
= 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-infrared radial velocities (RVs) with the Habitable-zone Planet Finder Spectrograph, ground-based photometry, and high-contrast imaging. A joint photometry and RV fit yields a radius
R
p
=
3.37
−
0.20
+
0.15
R
⊕
, mass
m
p
=
16.4
−
4.1
+
4.1
M
⊕
, and density
ρ
p
=
2.32
−
0.37
+
0.38
g
cm
−
3
for TOI-2015 b, suggesting a likely volatile-rich planet. The young, active host star has a rotation period of
P
rot
= 8.7 ± 0.9 days and associated rotation-based age estimate of 1.1 ± 0.1 Gyr. Though no other transiting planets are seen in the TESS data, the system shows clear TTVs of super-period
P
sup
≈
430
days
and amplitude ∼100 minutes. After considering multiple likely period-ratio models, we show an outer planet candidate near a 2:1 resonance can explain the observed TTVs while offering a dynamically stable solution. However, other possible two-planet solutions—including 3:2 and 4:3 resonances—cannot be conclusively excluded without further observations. Assuming a 2:1 resonance in the joint TTV-RV modeling suggests a mass of
m
b
=
13.3
−
4.5
+
4.7
M
⊕
for TOI-2015 b and
m
c
=
6.8
−
2.3
+
3.5
M
⊕
for the outer candidate. Additional transit and RV observations will be beneficial to explicitly identify the resonance and further characterize the properties of the system. |
| doi_str_mv | 10.3847/1538-3881/ad55ea |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_doaj_</sourceid><recordid>TN_cdi_proquest_journals_3085105105</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><doaj_id>oai_doaj_org_article_052ce9f7dd8e41bbb7f9ee8f3027d738</doaj_id><sourcerecordid>3085105105</sourcerecordid><originalsourceid>FETCH-LOGICAL-c299t-55e0676350eeb310d216226714e457d2c16315ce55da8f9457f04c5fc10fdd533</originalsourceid><addsrcrecordid>eNp1UU1LxDAQDaLgunr3GPBqdZI0beptWb8W1L2sepKQ5kOz7LY1zSr7722t6EkYmOHx3pvhDULHBM6YSPNzwplImBDkXBnOrdpBo19oF40AIE0yyrN9dNC2SwBCBKQj9LKYzxIKhOPyAk_wswpr_GCbuKks_vTxDS-Cqlof8cKvffWKn1TwKvq6avE8lD72mKrwREf_YfG9N0ncNt2ALz9VcIdoz6lVa49--hg9Xl8tprfJ3fxmNp3cJZoWRUy6eyHLM8bB2pIRMJRklGY5SW3Kc0M1yRjh2nJulHBFhzlINXeagDOGMzZGs8HX1Gopm-DXKmxlrbz8BurwKlWIXq-sBE61LVxujLApKcsyd4W1wjGgucmZ6LxOBq8m1O8b20a5rDeh6s6XDAQn0FfHgoGlQ922wbrfrQRk_xDZpy_79OXwkE5yOkh83fx5_kv_AohKiUc</addsrcrecordid><sourcetype>Open Website</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3085105105</pqid></control><display><type>article</type><title>TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf</title><source>IOP Publishing Free Content</source><source>DOAJ Directory of Open Access Journals</source><source>EZB-FREE-00999 freely available EZB journals</source><source>Alma/SFX Local Collection</source><creator>Jones, Sinclaire E. ; Stefánsson, Guđmundur ; Masuda, Kento ; Libby-Roberts, Jessica E. ; Gardner, Cristilyn N. ; Holcomb, Rae ; Beard, Corey ; Robertson, Paul ; Cañas, Caleb I. ; Mahadevan, Suvrath ; Kanodia, Shubham ; Lin, Andrea S. J. ; Kobulnicky, Henry A. ; Parker, Brock A. ; Bender, Chad F. ; Cochran, William D. ; Diddams, Scott A. ; Fernandes, Rachel B. ; Gupta, Arvind F. ; Halverson, Samuel ; Hawley, Suzanne L. ; Hearty, Fred R. ; Hebb, Leslie ; Kowalski, Adam ; Lubin, Jack ; Monson, Andrew ; Ninan, Joe P. ; Ramsey, Lawrence ; Roy, Arpita ; Schwab, Christian ; Terrien, Ryan C. ; Wisniewski, John</creator><creatorcontrib>Jones, Sinclaire E. ; Stefánsson, Guđmundur ; Masuda, Kento ; Libby-Roberts, Jessica E. ; Gardner, Cristilyn N. ; Holcomb, Rae ; Beard, Corey ; Robertson, Paul ; Cañas, Caleb I. ; Mahadevan, Suvrath ; Kanodia, Shubham ; Lin, Andrea S. J. ; Kobulnicky, Henry A. ; Parker, Brock A. ; Bender, Chad F. ; Cochran, William D. ; Diddams, Scott A. ; Fernandes, Rachel B. ; Gupta, Arvind F. ; Halverson, Samuel ; Hawley, Suzanne L. ; Hearty, Fred R. ; Hebb, Leslie ; Kowalski, Adam ; Lubin, Jack ; Monson, Andrew ; Ninan, Joe P. ; Ramsey, Lawrence ; Roy, Arpita ; Schwab, Christian ; Terrien, Ryan C. ; Wisniewski, John</creatorcontrib><description>We report the discovery of a close-in (
P
orb
= 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby (
d
= 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-infrared radial velocities (RVs) with the Habitable-zone Planet Finder Spectrograph, ground-based photometry, and high-contrast imaging. A joint photometry and RV fit yields a radius
R
p
=
3.37
−
0.20
+
0.15
R
⊕
, mass
m
p
=
16.4
−
4.1
+
4.1
M
⊕
, and density
ρ
p
=
2.32
−
0.37
+
0.38
g
cm
−
3
for TOI-2015 b, suggesting a likely volatile-rich planet. The young, active host star has a rotation period of
P
rot
= 8.7 ± 0.9 days and associated rotation-based age estimate of 1.1 ± 0.1 Gyr. Though no other transiting planets are seen in the TESS data, the system shows clear TTVs of super-period
P
sup
≈
430
days
and amplitude ∼100 minutes. After considering multiple likely period-ratio models, we show an outer planet candidate near a 2:1 resonance can explain the observed TTVs while offering a dynamically stable solution. However, other possible two-planet solutions—including 3:2 and 4:3 resonances—cannot be conclusively excluded without further observations. Assuming a 2:1 resonance in the joint TTV-RV modeling suggests a mass of
m
b
=
13.3
−
4.5
+
4.7
M
⊕
for TOI-2015 b and
m
c
=
6.8
−
2.3
+
3.5
M
⊕
for the outer candidate. Additional transit and RV observations will be beneficial to explicitly identify the resonance and further characterize the properties of the system.</description><identifier>ISSN: 0004-6256</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/ad55ea</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Circumstellar habitable zone ; Dynamic stability ; Exoplanets ; Extrasolar planets ; Gas giant planets ; Infrared photometry ; M dwarf stars ; Near infrared radiation ; Neptune ; Orbital resonances (celestial mechanics) ; Photometry ; Planet detection ; Planetary rotation ; Planets ; Radial velocity ; Resonance ; Transit ; Transit timing variation method ; Transits</subject><ispartof>The Astronomical journal, 2024-08, Vol.168 (2), p.93</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. 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><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c299t-55e0676350eeb310d216226714e457d2c16315ce55da8f9457f04c5fc10fdd533</cites><orcidid>0000-0001-8342-7736 ; 0000-0001-7409-5688 ; 0000-0003-1263-8637 ; 0000-0002-0048-2586 ; 0000-0001-8401-4300 ; 0000-0001-8127-5775 ; 0000-0001-7458-1176 ; 0000-0002-4289-7958 ; 0000-0001-8621-6731 ; 0000-0002-5463-9980 ; 0000-0003-1312-9391 ; 0000-0002-6629-4182 ; 0000-0003-4835-0619 ; 0000-0001-9209-1808 ; 0000-0001-9596-7983 ; 0000-0002-9082-6337 ; 0000-0001-9307-8170 ; 0000-0002-1664-3102 ; 0000-0002-3853-7327 ; 0000-0002-4788-8858 ; 0000-0001-9662-3496 ; 0000-0002-7227-2334 ; 0000-0003-4384-7220 ; 0000-0003-0149-9678 ; 0000-0002-4046-987X ; 0000-0003-1298-9699 ; 0000-0001-7708-2364 ; 0000-0002-2144-0764 ; 0000-0001-8720-5612 ; 0000-0002-5034-9476 ; 0000-0002-2990-7613 ; 0000-0002-4475-4176</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/ad55ea/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>Jones, Sinclaire E.</creatorcontrib><creatorcontrib>Stefánsson, Guđmundur</creatorcontrib><creatorcontrib>Masuda, Kento</creatorcontrib><creatorcontrib>Libby-Roberts, Jessica E.</creatorcontrib><creatorcontrib>Gardner, Cristilyn N.</creatorcontrib><creatorcontrib>Holcomb, Rae</creatorcontrib><creatorcontrib>Beard, Corey</creatorcontrib><creatorcontrib>Robertson, Paul</creatorcontrib><creatorcontrib>Cañas, Caleb I.</creatorcontrib><creatorcontrib>Mahadevan, Suvrath</creatorcontrib><creatorcontrib>Kanodia, Shubham</creatorcontrib><creatorcontrib>Lin, Andrea S. J.</creatorcontrib><creatorcontrib>Kobulnicky, Henry A.</creatorcontrib><creatorcontrib>Parker, Brock A.</creatorcontrib><creatorcontrib>Bender, Chad F.</creatorcontrib><creatorcontrib>Cochran, William D.</creatorcontrib><creatorcontrib>Diddams, Scott A.</creatorcontrib><creatorcontrib>Fernandes, Rachel B.</creatorcontrib><creatorcontrib>Gupta, Arvind F.</creatorcontrib><creatorcontrib>Halverson, Samuel</creatorcontrib><creatorcontrib>Hawley, Suzanne L.</creatorcontrib><creatorcontrib>Hearty, Fred R.</creatorcontrib><creatorcontrib>Hebb, Leslie</creatorcontrib><creatorcontrib>Kowalski, Adam</creatorcontrib><creatorcontrib>Lubin, Jack</creatorcontrib><creatorcontrib>Monson, Andrew</creatorcontrib><creatorcontrib>Ninan, Joe P.</creatorcontrib><creatorcontrib>Ramsey, Lawrence</creatorcontrib><creatorcontrib>Roy, Arpita</creatorcontrib><creatorcontrib>Schwab, Christian</creatorcontrib><creatorcontrib>Terrien, Ryan C.</creatorcontrib><creatorcontrib>Wisniewski, John</creatorcontrib><title>TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We report the discovery of a close-in (
P
orb
= 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby (
d
= 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-infrared radial velocities (RVs) with the Habitable-zone Planet Finder Spectrograph, ground-based photometry, and high-contrast imaging. A joint photometry and RV fit yields a radius
R
p
=
3.37
−
0.20
+
0.15
R
⊕
, mass
m
p
=
16.4
−
4.1
+
4.1
M
⊕
, and density
ρ
p
=
2.32
−
0.37
+
0.38
g
cm
−
3
for TOI-2015 b, suggesting a likely volatile-rich planet. The young, active host star has a rotation period of
P
rot
= 8.7 ± 0.9 days and associated rotation-based age estimate of 1.1 ± 0.1 Gyr. Though no other transiting planets are seen in the TESS data, the system shows clear TTVs of super-period
P
sup
≈
430
days
and amplitude ∼100 minutes. After considering multiple likely period-ratio models, we show an outer planet candidate near a 2:1 resonance can explain the observed TTVs while offering a dynamically stable solution. However, other possible two-planet solutions—including 3:2 and 4:3 resonances—cannot be conclusively excluded without further observations. Assuming a 2:1 resonance in the joint TTV-RV modeling suggests a mass of
m
b
=
13.3
−
4.5
+
4.7
M
⊕
for TOI-2015 b and
m
c
=
6.8
−
2.3
+
3.5
M
⊕
for the outer candidate. Additional transit and RV observations will be beneficial to explicitly identify the resonance and further characterize the properties of the system.</description><subject>Circumstellar habitable zone</subject><subject>Dynamic stability</subject><subject>Exoplanets</subject><subject>Extrasolar planets</subject><subject>Gas giant planets</subject><subject>Infrared photometry</subject><subject>M dwarf stars</subject><subject>Near infrared radiation</subject><subject>Neptune</subject><subject>Orbital resonances (celestial mechanics)</subject><subject>Photometry</subject><subject>Planet detection</subject><subject>Planetary rotation</subject><subject>Planets</subject><subject>Radial velocity</subject><subject>Resonance</subject><subject>Transit</subject><subject>Transit timing variation method</subject><subject>Transits</subject><issn>0004-6256</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1UU1LxDAQDaLgunr3GPBqdZI0beptWb8W1L2sepKQ5kOz7LY1zSr7722t6EkYmOHx3pvhDULHBM6YSPNzwplImBDkXBnOrdpBo19oF40AIE0yyrN9dNC2SwBCBKQj9LKYzxIKhOPyAk_wswpr_GCbuKks_vTxDS-Cqlof8cKvffWKn1TwKvq6avE8lD72mKrwREf_YfG9N0ncNt2ALz9VcIdoz6lVa49--hg9Xl8tprfJ3fxmNp3cJZoWRUy6eyHLM8bB2pIRMJRklGY5SW3Kc0M1yRjh2nJulHBFhzlINXeagDOGMzZGs8HX1Gopm-DXKmxlrbz8BurwKlWIXq-sBE61LVxujLApKcsyd4W1wjGgucmZ6LxOBq8m1O8b20a5rDeh6s6XDAQn0FfHgoGlQ922wbrfrQRk_xDZpy_79OXwkE5yOkh83fx5_kv_AohKiUc</recordid><startdate>20240801</startdate><enddate>20240801</enddate><creator>Jones, Sinclaire E.</creator><creator>Stefánsson, Guđmundur</creator><creator>Masuda, Kento</creator><creator>Libby-Roberts, Jessica E.</creator><creator>Gardner, Cristilyn N.</creator><creator>Holcomb, Rae</creator><creator>Beard, Corey</creator><creator>Robertson, Paul</creator><creator>Cañas, Caleb I.</creator><creator>Mahadevan, Suvrath</creator><creator>Kanodia, Shubham</creator><creator>Lin, Andrea S. J.</creator><creator>Kobulnicky, Henry A.</creator><creator>Parker, Brock A.</creator><creator>Bender, Chad F.</creator><creator>Cochran, William D.</creator><creator>Diddams, Scott A.</creator><creator>Fernandes, Rachel B.</creator><creator>Gupta, Arvind F.</creator><creator>Halverson, Samuel</creator><creator>Hawley, Suzanne L.</creator><creator>Hearty, Fred R.</creator><creator>Hebb, Leslie</creator><creator>Kowalski, Adam</creator><creator>Lubin, Jack</creator><creator>Monson, Andrew</creator><creator>Ninan, Joe P.</creator><creator>Ramsey, Lawrence</creator><creator>Roy, Arpita</creator><creator>Schwab, Christian</creator><creator>Terrien, Ryan C.</creator><creator>Wisniewski, John</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0001-8342-7736</orcidid><orcidid>https://orcid.org/0000-0001-7409-5688</orcidid><orcidid>https://orcid.org/0000-0003-1263-8637</orcidid><orcidid>https://orcid.org/0000-0002-0048-2586</orcidid><orcidid>https://orcid.org/0000-0001-8401-4300</orcidid><orcidid>https://orcid.org/0000-0001-8127-5775</orcidid><orcidid>https://orcid.org/0000-0001-7458-1176</orcidid><orcidid>https://orcid.org/0000-0002-4289-7958</orcidid><orcidid>https://orcid.org/0000-0001-8621-6731</orcidid><orcidid>https://orcid.org/0000-0002-5463-9980</orcidid><orcidid>https://orcid.org/0000-0003-1312-9391</orcidid><orcidid>https://orcid.org/0000-0002-6629-4182</orcidid><orcidid>https://orcid.org/0000-0003-4835-0619</orcidid><orcidid>https://orcid.org/0000-0001-9209-1808</orcidid><orcidid>https://orcid.org/0000-0001-9596-7983</orcidid><orcidid>https://orcid.org/0000-0002-9082-6337</orcidid><orcidid>https://orcid.org/0000-0001-9307-8170</orcidid><orcidid>https://orcid.org/0000-0002-1664-3102</orcidid><orcidid>https://orcid.org/0000-0002-3853-7327</orcidid><orcidid>https://orcid.org/0000-0002-4788-8858</orcidid><orcidid>https://orcid.org/0000-0001-9662-3496</orcidid><orcidid>https://orcid.org/0000-0002-7227-2334</orcidid><orcidid>https://orcid.org/0000-0003-4384-7220</orcidid><orcidid>https://orcid.org/0000-0003-0149-9678</orcidid><orcidid>https://orcid.org/0000-0002-4046-987X</orcidid><orcidid>https://orcid.org/0000-0003-1298-9699</orcidid><orcidid>https://orcid.org/0000-0001-7708-2364</orcidid><orcidid>https://orcid.org/0000-0002-2144-0764</orcidid><orcidid>https://orcid.org/0000-0001-8720-5612</orcidid><orcidid>https://orcid.org/0000-0002-5034-9476</orcidid><orcidid>https://orcid.org/0000-0002-2990-7613</orcidid><orcidid>https://orcid.org/0000-0002-4475-4176</orcidid></search><sort><creationdate>20240801</creationdate><title>TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf</title><author>Jones, Sinclaire E. ; Stefánsson, Guđmundur ; Masuda, Kento ; Libby-Roberts, Jessica E. ; Gardner, Cristilyn N. ; Holcomb, Rae ; Beard, Corey ; Robertson, Paul ; Cañas, Caleb I. ; Mahadevan, Suvrath ; Kanodia, Shubham ; Lin, Andrea S. J. ; Kobulnicky, Henry A. ; Parker, Brock A. ; Bender, Chad F. ; Cochran, William D. ; Diddams, Scott A. ; Fernandes, Rachel B. ; Gupta, Arvind F. ; Halverson, Samuel ; Hawley, Suzanne L. ; Hearty, Fred R. ; Hebb, Leslie ; Kowalski, Adam ; Lubin, Jack ; Monson, Andrew ; Ninan, Joe P. ; Ramsey, Lawrence ; Roy, Arpita ; Schwab, Christian ; Terrien, Ryan C. ; Wisniewski, John</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c299t-55e0676350eeb310d216226714e457d2c16315ce55da8f9457f04c5fc10fdd533</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Circumstellar habitable zone</topic><topic>Dynamic stability</topic><topic>Exoplanets</topic><topic>Extrasolar planets</topic><topic>Gas giant planets</topic><topic>Infrared photometry</topic><topic>M dwarf stars</topic><topic>Near infrared radiation</topic><topic>Neptune</topic><topic>Orbital resonances (celestial mechanics)</topic><topic>Photometry</topic><topic>Planet detection</topic><topic>Planetary rotation</topic><topic>Planets</topic><topic>Radial velocity</topic><topic>Resonance</topic><topic>Transit</topic><topic>Transit timing variation method</topic><topic>Transits</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Jones, Sinclaire E.</creatorcontrib><creatorcontrib>Stefánsson, Guđmundur</creatorcontrib><creatorcontrib>Masuda, Kento</creatorcontrib><creatorcontrib>Libby-Roberts, Jessica E.</creatorcontrib><creatorcontrib>Gardner, Cristilyn N.</creatorcontrib><creatorcontrib>Holcomb, Rae</creatorcontrib><creatorcontrib>Beard, Corey</creatorcontrib><creatorcontrib>Robertson, Paul</creatorcontrib><creatorcontrib>Cañas, Caleb I.</creatorcontrib><creatorcontrib>Mahadevan, Suvrath</creatorcontrib><creatorcontrib>Kanodia, Shubham</creatorcontrib><creatorcontrib>Lin, Andrea S. J.</creatorcontrib><creatorcontrib>Kobulnicky, Henry A.</creatorcontrib><creatorcontrib>Parker, Brock A.</creatorcontrib><creatorcontrib>Bender, Chad F.</creatorcontrib><creatorcontrib>Cochran, William D.</creatorcontrib><creatorcontrib>Diddams, Scott A.</creatorcontrib><creatorcontrib>Fernandes, Rachel B.</creatorcontrib><creatorcontrib>Gupta, Arvind F.</creatorcontrib><creatorcontrib>Halverson, Samuel</creatorcontrib><creatorcontrib>Hawley, Suzanne L.</creatorcontrib><creatorcontrib>Hearty, Fred R.</creatorcontrib><creatorcontrib>Hebb, Leslie</creatorcontrib><creatorcontrib>Kowalski, Adam</creatorcontrib><creatorcontrib>Lubin, Jack</creatorcontrib><creatorcontrib>Monson, Andrew</creatorcontrib><creatorcontrib>Ninan, Joe P.</creatorcontrib><creatorcontrib>Ramsey, Lawrence</creatorcontrib><creatorcontrib>Roy, Arpita</creatorcontrib><creatorcontrib>Schwab, Christian</creatorcontrib><creatorcontrib>Terrien, Ryan C.</creatorcontrib><creatorcontrib>Wisniewski, John</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>The Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Jones, Sinclaire E.</au><au>Stefánsson, Guđmundur</au><au>Masuda, Kento</au><au>Libby-Roberts, Jessica E.</au><au>Gardner, Cristilyn N.</au><au>Holcomb, Rae</au><au>Beard, Corey</au><au>Robertson, Paul</au><au>Cañas, Caleb I.</au><au>Mahadevan, Suvrath</au><au>Kanodia, Shubham</au><au>Lin, Andrea S. J.</au><au>Kobulnicky, Henry A.</au><au>Parker, Brock A.</au><au>Bender, Chad F.</au><au>Cochran, William D.</au><au>Diddams, Scott A.</au><au>Fernandes, Rachel B.</au><au>Gupta, Arvind F.</au><au>Halverson, Samuel</au><au>Hawley, Suzanne L.</au><au>Hearty, Fred R.</au><au>Hebb, Leslie</au><au>Kowalski, Adam</au><au>Lubin, Jack</au><au>Monson, Andrew</au><au>Ninan, Joe P.</au><au>Ramsey, Lawrence</au><au>Roy, Arpita</au><au>Schwab, Christian</au><au>Terrien, Ryan C.</au><au>Wisniewski, John</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2024-08-01</date><risdate>2024</risdate><volume>168</volume><issue>2</issue><spage>93</spage><pages>93-</pages><issn>0004-6256</issn><eissn>1538-3881</eissn><abstract>We report the discovery of a close-in (
P
orb
= 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby (
d
= 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-infrared radial velocities (RVs) with the Habitable-zone Planet Finder Spectrograph, ground-based photometry, and high-contrast imaging. A joint photometry and RV fit yields a radius
R
p
=
3.37
−
0.20
+
0.15
R
⊕
, mass
m
p
=
16.4
−
4.1
+
4.1
M
⊕
, and density
ρ
p
=
2.32
−
0.37
+
0.38
g
cm
−
3
for TOI-2015 b, suggesting a likely volatile-rich planet. The young, active host star has a rotation period of
P
rot
= 8.7 ± 0.9 days and associated rotation-based age estimate of 1.1 ± 0.1 Gyr. Though no other transiting planets are seen in the TESS data, the system shows clear TTVs of super-period
P
sup
≈
430
days
and amplitude ∼100 minutes. After considering multiple likely period-ratio models, we show an outer planet candidate near a 2:1 resonance can explain the observed TTVs while offering a dynamically stable solution. However, other possible two-planet solutions—including 3:2 and 4:3 resonances—cannot be conclusively excluded without further observations. Assuming a 2:1 resonance in the joint TTV-RV modeling suggests a mass of
m
b
=
13.3
−
4.5
+
4.7
M
⊕
for TOI-2015 b and
m
c
=
6.8
−
2.3
+
3.5
M
⊕
for the outer candidate. Additional transit and RV observations will be beneficial to explicitly identify the resonance and further characterize the properties of the system.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/ad55ea</doi><tpages>24</tpages><orcidid>https://orcid.org/0000-0001-8342-7736</orcidid><orcidid>https://orcid.org/0000-0001-7409-5688</orcidid><orcidid>https://orcid.org/0000-0003-1263-8637</orcidid><orcidid>https://orcid.org/0000-0002-0048-2586</orcidid><orcidid>https://orcid.org/0000-0001-8401-4300</orcidid><orcidid>https://orcid.org/0000-0001-8127-5775</orcidid><orcidid>https://orcid.org/0000-0001-7458-1176</orcidid><orcidid>https://orcid.org/0000-0002-4289-7958</orcidid><orcidid>https://orcid.org/0000-0001-8621-6731</orcidid><orcidid>https://orcid.org/0000-0002-5463-9980</orcidid><orcidid>https://orcid.org/0000-0003-1312-9391</orcidid><orcidid>https://orcid.org/0000-0002-6629-4182</orcidid><orcidid>https://orcid.org/0000-0003-4835-0619</orcidid><orcidid>https://orcid.org/0000-0001-9209-1808</orcidid><orcidid>https://orcid.org/0000-0001-9596-7983</orcidid><orcidid>https://orcid.org/0000-0002-9082-6337</orcidid><orcidid>https://orcid.org/0000-0001-9307-8170</orcidid><orcidid>https://orcid.org/0000-0002-1664-3102</orcidid><orcidid>https://orcid.org/0000-0002-3853-7327</orcidid><orcidid>https://orcid.org/0000-0002-4788-8858</orcidid><orcidid>https://orcid.org/0000-0001-9662-3496</orcidid><orcidid>https://orcid.org/0000-0002-7227-2334</orcidid><orcidid>https://orcid.org/0000-0003-4384-7220</orcidid><orcidid>https://orcid.org/0000-0003-0149-9678</orcidid><orcidid>https://orcid.org/0000-0002-4046-987X</orcidid><orcidid>https://orcid.org/0000-0003-1298-9699</orcidid><orcidid>https://orcid.org/0000-0001-7708-2364</orcidid><orcidid>https://orcid.org/0000-0002-2144-0764</orcidid><orcidid>https://orcid.org/0000-0001-8720-5612</orcidid><orcidid>https://orcid.org/0000-0002-5034-9476</orcidid><orcidid>https://orcid.org/0000-0002-2990-7613</orcidid><orcidid>https://orcid.org/0000-0002-4475-4176</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6256 |
| ispartof | The Astronomical journal, 2024-08, Vol.168 (2), p.93 |
| issn | 0004-6256 1538-3881 |
| language | eng |
| recordid | cdi_proquest_journals_3085105105 |
| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Circumstellar habitable zone Dynamic stability Exoplanets Extrasolar planets Gas giant planets Infrared photometry M dwarf stars Near infrared radiation Neptune Orbital resonances (celestial mechanics) Photometry Planet detection Planetary rotation Planets Radial velocity Resonance Transit Transit timing variation method Transits |
| title | TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-08T12%3A31%3A16IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_doaj_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=TOI-2015%20b:%20A%20Warm%20Neptune%20with%20Transit%20Timing%20Variations%20Orbiting%20an%20Active%20Mid-type%20M%20Dwarf&rft.jtitle=The%20Astronomical%20journal&rft.au=Jones,%20Sinclaire%20E.&rft.date=2024-08-01&rft.volume=168&rft.issue=2&rft.spage=93&rft.pages=93-&rft.issn=0004-6256&rft.eissn=1538-3881&rft_id=info:doi/10.3847/1538-3881/ad55ea&rft_dat=%3Cproquest_doaj_%3E3085105105%3C/proquest_doaj_%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=3085105105&rft_id=info:pmid/&rft_doaj_id=oai_doaj_org_article_052ce9f7dd8e41bbb7f9ee8f3027d738&rfr_iscdi=true |