TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes

Fei Dai; Andrew W. Howard; Natalie M. Batalha; Corey Beard; Aida Behmard; Sarah Blunt; Casey L. Brinkman; Ashley Chontos; Ian J.M. Crossfield; Paul A. Dalba; Courtney Dressing; Benjamin Fulton; Steven Giacalone; Michelle L. Hill; Daniel Huber; Howard Isaacson; Stephen R. Kane; Jack Lubin; Andrew Mayo; Teo Močnik; Joseph M. Akana Murphy; Erik A. Petigura; Malena Rice; Paul Robertson; Lee Rosenthal; Arpita Roy; Ryan A. Rubenzahl; Lauren M. Weiss; Judah Van Zandt; Charles Beichman; David Ciardi; Karen A. Collins; Erica Gonzales; Steve B. Howell; Rachel A. Matson; Elisabeth C. Matthews; Joshua E. Schlieder; Richard P. Schwarz; George R. Ricker; Roland Vanderspek; David W. Latham; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Douglas A. Caldwell; Knicole D. Colon; Diana Dragomir; Michael B. Lund; Brian McLean; Alexander Rudat; Avi Shporer

doi:10.3847/1538-3881/ac02bd

TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes

Fei Dai, Andrew W. Howard, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Ian J.M. Crossfield, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Andrew Mayo, Teo MočnikJoseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Paul Robertson, Lee Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Judah Van Zandt, Charles Beichman, David Ciardi, Karen A. Collins, Erica Gonzales, Steve B. Howell, Rachel A. Matson, Elisabeth C. Matthews, Joshua E. Schlieder, Richard P. Schwarz, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Douglas A. Caldwell, Knicole D. Colon, Diana Dragomir, Michael B. Lund, Brian McLean, Alexander Rudat, Avi Shporer

Astrophysical Sciences

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Abstract

We report the discovery of TOI-1444b, a 1.4 R ⊕ super-Earth on a 0.47 day orbit around a Sun-like star discovered by TESS. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ± 0.71M ⊕. The RV data set also indicates a possible nontransiting, 16 day planet (11.8 ± 2.9M ⊕). We report a tentative detection of phase-curve variation and a secondary eclipse of TOI-1444b in the TESS bandpass. TOI-1444b joins the growing sample of 17 ultra-short-period planets (USPs) with well-measured masses and sizes, most of which are compatible with an Earth-like composition. We take this opportunity to examine the expanding sample of ultra-short-period planets (<2R ⊕) and contrast them with the newly discovered sub-day ultrahot Neptunes (>3R ⊕, >2000F ⊕ TOI-849 b, LTT9779 b, and K2-100). We find that (1) USPs have predominately Earth-like compositions with inferred iron core mass fractions of 0.32 ± 0.04 and have masses below the threshold of runaway accretion (∼10M ⊕), while ultrahot Neptunes are above the threshold and have H/He or other volatile envelopes. (2) USPs are almost always found in multi-planet systems consistent with a secular interaction formation scenario; ultrahot Neptunes (P orb ≲1 day) tend to be "lonely,"similar to longer-period hot Neptunes (P orb1-10 days) and hot Jupiters. (3) USPs occur around solar-metallicity stars while hot Neptunes prefer higher metallicity hosts. (4) In all these respects, ultrahot Neptunes show more resemblance to hot Jupiters than the smaller USP planets, although ultrahot Neptunes are rarer than both USPs and hot Jupiters by 1-2 orders of magnitude.

Original language	English (US)
Article number	62
Journal	Astronomical Journal
Volume	162
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/ac02bd
State	Published - Aug 2021

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-3881/ac02bd

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Dai, F., Howard, A. W., Batalha, N. M., Beard, C., Behmard, A., Blunt, S., Brinkman, C. L., Chontos, A., Crossfield, I. J. M., Dalba, P. A., Dressing, C., Fulton, B., Giacalone, S., Hill, M. L., Huber, D., Isaacson, H., Kane, S. R., Lubin, J., Mayo, A., ... Shporer, A. (2021). TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes. Astronomical Journal, 162(2), Article 62. https://doi.org/10.3847/1538-3881/ac02bd

@article{4b425a8c367740afb4ca52583b1ee162,

title = "TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes",

abstract = "We report the discovery of TOI-1444b, a 1.4 R ⊕ super-Earth on a 0.47 day orbit around a Sun-like star discovered by TESS. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ± 0.71M ⊕. The RV data set also indicates a possible nontransiting, 16 day planet (11.8 ± 2.9M ⊕). We report a tentative detection of phase-curve variation and a secondary eclipse of TOI-1444b in the TESS bandpass. TOI-1444b joins the growing sample of 17 ultra-short-period planets (USPs) with well-measured masses and sizes, most of which are compatible with an Earth-like composition. We take this opportunity to examine the expanding sample of ultra-short-period planets (<2R ⊕) and contrast them with the newly discovered sub-day ultrahot Neptunes (>3R ⊕, >2000F ⊕ TOI-849 b, LTT9779 b, and K2-100). We find that (1) USPs have predominately Earth-like compositions with inferred iron core mass fractions of 0.32 ± 0.04 and have masses below the threshold of runaway accretion (∼10M ⊕), while ultrahot Neptunes are above the threshold and have H/He or other volatile envelopes. (2) USPs are almost always found in multi-planet systems consistent with a secular interaction formation scenario; ultrahot Neptunes (P orb ≲1 day) tend to be {"}lonely,{"}similar to longer-period hot Neptunes (P orb1-10 days) and hot Jupiters. (3) USPs occur around solar-metallicity stars while hot Neptunes prefer higher metallicity hosts. (4) In all these respects, ultrahot Neptunes show more resemblance to hot Jupiters than the smaller USP planets, although ultrahot Neptunes are rarer than both USPs and hot Jupiters by 1-2 orders of magnitude.",

author = "Fei Dai and Howard, {Andrew W.} and Batalha, {Natalie M.} and Corey Beard and Aida Behmard and Sarah Blunt and Brinkman, {Casey L.} and Ashley Chontos and Crossfield, {Ian J.M.} and Dalba, {Paul A.} and Courtney Dressing and Benjamin Fulton and Steven Giacalone and Hill, {Michelle L.} and Daniel Huber and Howard Isaacson and Kane, {Stephen R.} and Jack Lubin and Andrew Mayo and Teo Mo{\v c}nik and {Akana Murphy}, {Joseph M.} and Petigura, {Erik A.} and Malena Rice and Paul Robertson and Lee Rosenthal and Arpita Roy and Rubenzahl, {Ryan A.} and Weiss, {Lauren M.} and Zandt, {Judah Van} and Charles Beichman and David Ciardi and Collins, {Karen A.} and Erica Gonzales and Howell, {Steve B.} and Matson, {Rachel A.} and Matthews, {Elisabeth C.} and Schlieder, {Joshua E.} and Schwarz, {Richard P.} and Ricker, {George R.} and Roland Vanderspek and Latham, {David W.} and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Caldwell, {Douglas A.} and Colon, {Knicole D.} and Diana Dragomir and Lund, {Michael B.} and Brian McLean and Alexander Rudat and Avi Shporer",

year = "2021",

month = aug,

doi = "10.3847/1538-3881/ac02bd",

language = "English (US)",

volume = "162",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "2",

}

Dai, F, Howard, AW, Batalha, NM, Beard, C, Behmard, A, Blunt, S, Brinkman, CL, Chontos, A, Crossfield, IJM, Dalba, PA, Dressing, C, Fulton, B, Giacalone, S, Hill, ML, Huber, D, Isaacson, H, Kane, SR, Lubin, J, Mayo, A, Močnik, T, Akana Murphy, JM, Petigura, EA, Rice, M, Robertson, P, Rosenthal, L, Roy, A, Rubenzahl, RA, Weiss, LM, Zandt, JV, Beichman, C, Ciardi, D, Collins, KA, Gonzales, E, Howell, SB, Matson, RA, Matthews, EC, Schlieder, JE, Schwarz, RP, Ricker, GR, Vanderspek, R, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Caldwell, DA, Colon, KD, Dragomir, D, Lund, MB, McLean, B, Rudat, A & Shporer, A 2021, 'TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes', Astronomical Journal, vol. 162, no. 2, 62. https://doi.org/10.3847/1538-3881/ac02bd

TY - JOUR

T1 - TKS X

T2 - Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes

AU - Dai, Fei

AU - Howard, Andrew W.

AU - Batalha, Natalie M.

AU - Beard, Corey

AU - Behmard, Aida

AU - Blunt, Sarah

AU - Brinkman, Casey L.

AU - Chontos, Ashley

AU - Crossfield, Ian J.M.

AU - Dalba, Paul A.

AU - Dressing, Courtney

AU - Fulton, Benjamin

AU - Giacalone, Steven

AU - Hill, Michelle L.

AU - Huber, Daniel

AU - Isaacson, Howard

AU - Kane, Stephen R.

AU - Lubin, Jack

AU - Mayo, Andrew

AU - Močnik, Teo

AU - Akana Murphy, Joseph M.

AU - Petigura, Erik A.

AU - Rice, Malena

AU - Robertson, Paul

AU - Rosenthal, Lee

AU - Roy, Arpita

AU - Rubenzahl, Ryan A.

AU - Weiss, Lauren M.

AU - Zandt, Judah Van

AU - Beichman, Charles

AU - Ciardi, David

AU - Collins, Karen A.

AU - Gonzales, Erica

AU - Howell, Steve B.

AU - Matson, Rachel A.

AU - Matthews, Elisabeth C.

AU - Schlieder, Joshua E.

AU - Schwarz, Richard P.

AU - Ricker, George R.

AU - Vanderspek, Roland

AU - Latham, David W.

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Caldwell, Douglas A.

AU - Colon, Knicole D.

AU - Dragomir, Diana

AU - Lund, Michael B.

AU - McLean, Brian

AU - Rudat, Alexander

AU - Shporer, Avi

PY - 2021/8

Y1 - 2021/8

N2 - We report the discovery of TOI-1444b, a 1.4 R ⊕ super-Earth on a 0.47 day orbit around a Sun-like star discovered by TESS. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ± 0.71M ⊕. The RV data set also indicates a possible nontransiting, 16 day planet (11.8 ± 2.9M ⊕). We report a tentative detection of phase-curve variation and a secondary eclipse of TOI-1444b in the TESS bandpass. TOI-1444b joins the growing sample of 17 ultra-short-period planets (USPs) with well-measured masses and sizes, most of which are compatible with an Earth-like composition. We take this opportunity to examine the expanding sample of ultra-short-period planets (<2R ⊕) and contrast them with the newly discovered sub-day ultrahot Neptunes (>3R ⊕, >2000F ⊕ TOI-849 b, LTT9779 b, and K2-100). We find that (1) USPs have predominately Earth-like compositions with inferred iron core mass fractions of 0.32 ± 0.04 and have masses below the threshold of runaway accretion (∼10M ⊕), while ultrahot Neptunes are above the threshold and have H/He or other volatile envelopes. (2) USPs are almost always found in multi-planet systems consistent with a secular interaction formation scenario; ultrahot Neptunes (P orb ≲1 day) tend to be "lonely,"similar to longer-period hot Neptunes (P orb1-10 days) and hot Jupiters. (3) USPs occur around solar-metallicity stars while hot Neptunes prefer higher metallicity hosts. (4) In all these respects, ultrahot Neptunes show more resemblance to hot Jupiters than the smaller USP planets, although ultrahot Neptunes are rarer than both USPs and hot Jupiters by 1-2 orders of magnitude.

AB - We report the discovery of TOI-1444b, a 1.4 R ⊕ super-Earth on a 0.47 day orbit around a Sun-like star discovered by TESS. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ± 0.71M ⊕. The RV data set also indicates a possible nontransiting, 16 day planet (11.8 ± 2.9M ⊕). We report a tentative detection of phase-curve variation and a secondary eclipse of TOI-1444b in the TESS bandpass. TOI-1444b joins the growing sample of 17 ultra-short-period planets (USPs) with well-measured masses and sizes, most of which are compatible with an Earth-like composition. We take this opportunity to examine the expanding sample of ultra-short-period planets (<2R ⊕) and contrast them with the newly discovered sub-day ultrahot Neptunes (>3R ⊕, >2000F ⊕ TOI-849 b, LTT9779 b, and K2-100). We find that (1) USPs have predominately Earth-like compositions with inferred iron core mass fractions of 0.32 ± 0.04 and have masses below the threshold of runaway accretion (∼10M ⊕), while ultrahot Neptunes are above the threshold and have H/He or other volatile envelopes. (2) USPs are almost always found in multi-planet systems consistent with a secular interaction formation scenario; ultrahot Neptunes (P orb ≲1 day) tend to be "lonely,"similar to longer-period hot Neptunes (P orb1-10 days) and hot Jupiters. (3) USPs occur around solar-metallicity stars while hot Neptunes prefer higher metallicity hosts. (4) In all these respects, ultrahot Neptunes show more resemblance to hot Jupiters than the smaller USP planets, although ultrahot Neptunes are rarer than both USPs and hot Jupiters by 1-2 orders of magnitude.

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ER -

TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes

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