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A Hot Mini-Neptune in the Radius Valley Orbiting Solar Analogue HD 110113

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A Hot Mini-Neptune in the Radius Valley Orbiting Solar Analogue HD 110113 MNRAS 000,1–15 (2021) Preprint 14 January 2021 Compiled using MNRAS LATEX style file v3.0 A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113 H.P. Osborn1,2, ¢, D.J. Armstrong3,4, , V. Adibekyan5, , K.A. Collins6, , E. Delgado-Mena5, , S.B. Howell7, , C. Hellier8, , G.W. King3,4, , J. Lillo- Box9, , L.D. Nielsen10, , J.F. Otegi10, N.C. Santos5,11, , C. Ziegler12, D.R. Anderson3,4, , C. Briceño13, , C. Burke2, , D. Bayliss4,3, , D. Barrado9, , E.M. Bryant4,3, , D.J.A. Brown3,4, , S.C.C. Barros5,11, , F. Bouchy10, , D.A. Caldwell14, , D.M. Conti15, , R.F. Díaz16, , D. Dragomir17, , M. Deleuil18, , O.D.S. Demangeon5,11, , C. Dorn19, , T. Daylan2,20, , P. Figueira21,5, , R. Helled19, , S. Hoyer18, , J.M. Jenkins7, , E.L.N. Jensen22, , D.W. Latham6, , N. Law23, D.R. Louie24, , A.W. Mann23, , A. Osborn4,3, , D.L. Pollacco4, , D.R. Rodriguez25, , B.V. Rackham2,26, , G. Ricker2, , N.J. Scott7, , S.G. Sousa5, , S. Seager2,26, , K.G. Stassun27, , J.C. Smith14, , P. Strøm4,3, , S. Udry10, , J. Villaseñor2, , R. Vanderspek2, , R. West3,4, P.J. Wheatley3,4, , J.N. Winn28, The authors’ affiliations are shown in AppendixA. Accepted 07-Jan-2021 ABSTRACT We report the discovery of HD 110113 b (TOI-755.01), a transiting mini-Neptune exoplanet on a 2.5-day orbit around the solar-analogue HD 110113 ()eff= 5730K). Using TESS photometry and HARPS radial velocities gathered by the NCORES program, we find HD 110113 b has a radius of 2.05 ± 0.12 R⊕ and a mass of 4.55 ± 0.62 M⊕. The resulting density of ¸0.75 −3 2.90−0.59 g cm is significantly lower than would be expected from a pure-rock world; therefore, HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. The high incident flux places it within the so-called radius valley; however, HD 110113 b was able to hold onto a substantial (0.1-1%) H-He atmosphere over its ∼ 4Gyr lifetime. Through a novel simultaneous gaussian process fit to multiple activity indicators, we were also able to fit for the strong stellar rotation signal with period 20.8 ± 1.2 d from the RVs and confirm an ± ¸0.008 additional non-transiting planet with a mass of 10.5 1.2 M⊕ and a period of 6.744−0.009 d. Key words: planets and satellites: detection – stars: individual: HD110113 arXiv:2101.04745v1 [astro-ph.EP] 12 Jan 2021 1 INTRODUCTION This unique combination of space-based photometry (which provides planetary radius) and precise radial velocities (which pro- Since its launch in 2018, NASA’s TESS mission has attempted to de- vide planetary mass) also allows for the determination of exoplanet tect small transiting planets around bright, nearby stars amenable to densities, and, therefore, an insight into the internal structure of confirmation with radial velocity observations (Ricker et al. 2016). worlds outside our solar system. These analyses have revealed a The HARPS spectrograph on the 3.6m telescope at La Silla, Chile diversity of planet structures in the regime between Earth and Nep- (Mayor et al. 2003) has been deeply involved in this follow-up effort, tune, from high-density evaporated giant planet cores like TOI-849b beginning with its first detection, the hot super-Earth Pi Mensae c (5.2 g cm−3 Armstrong et al. 2020), to low-density mini-Neptunes (Huang et al. 2018), and continuing with the first multi-planet sys- such as TOI-421 c (Carleo et al. 2020), as well as planets which tem (TOI-125 Quinn et al. 2019; Nielsen et al. 2020), follow a more linear track from rocky super-earths to Neptunes dominated by gaseous envelopes, such as the two inner planets or- ¢ E-mail: [email protected] © 2021 The Authors 2 H.P. Osborn et al. 25 2 TIC 73228647 - Sector 10 biting a Lupi (Kane et al. 2020) and TOI-735 (Cloutier et al. 2020; 1200 m = -2 7 Nowak et al. 2020). 21 6 m = 0 14 The detection of exoplanets with well-constrained physical pa- m = 2 5 m = 4 rameters can also lead to the discovery of statistical trends within 1198 4 m = 6 the planet population which encode information on planetary for- 19 m = 8 6 mation and evolution. The "valley" seen around 1.8 R⊕ in Kepler 24 4 8 26 2 3 9 ) 1196 data (Fulton et al. 2017; Van Eylen et al. 2018) is one such feature. 17 3 5 e 1 ( According to current theory planets that first formed with gaseous 22 15 3 envelopes within this valley have, due to heating from either their 0 1 1194 13 stars (e.g. evaporation, Owen & Wu 2017) or from internal sources × (e.g. core-powered mass loss, Ginzburg et al. 2018), lost those initial 12 x 23 u 7 l gaseous envelopes, thereby evolving to significantly smaller radii to F 16 become "evaporated cores". By observing the physical parameters Pixel Row Number 1192 11 10 of small, hot exoplanets, the exact mechanisms of this process can 18 be revealed. 20 E In this paper, we present the detection, confirmation and RV 1190 N characterisation of two exoplanets orbiting the star HD 110113 — the hot mini-Neptune HD 110113 b and the non-transiting 714 712 710 708 706 704 HD 110113 c. The observations from which these planets were de- Pixel Column Number tected are described in section2, while the analysis of that data is tpfplotter described in section3. In section4 we discuss the validity of the Figure 1. TESS photometric aperture plotted with (Aller et al. 2020). The default TESS aperture used by SAP is overplotted in red, and outer planet RV signal (4.1), whether HD 110113 is a solar ana- nearby stars down to Δmag = 8 from Gaia DR2 (Brown et al. 2018) are logue (4.2) the internal structure and evaporation of planet b (4.3 plotted as red circles. The target HD 110113 is marked with a white cross. & 4.4), and potential future observations of the system (4.5). We summarize our conclusions in section5. also ¡ 1 pixel away, and are increasingly fainter (Δmag of 6.9–7.9), requiring eclipse depths of 25–75%. Causing the observed transit with such a blend scenario therefore becomes increasingly unlikely 2 OBSERVATIONS given the flat-bottomed transit shape of TOI-755.01. We conclude 2.1 TESS photometry that a blend scenario from a known contaminant is unlikely, however we pursue additional photometry to confirm. HD 110113 was observed during TESS sector 10 with 2-minute ca- dence for 22.5 days, excluding a 2.5 day gap between TESS orbits to downlink data. The lightcurve was extracted using the SPOC 2.2 Ground-based Photometric Follow-up (Science Processing Operations Centre; Jenkins et al. 2016) SAP (simple aperture photometry) pipeline. It was then processed us- We observed a full transit of TOI-755.01 continuously for 443 min- ing the Pre-Search Data Conditioning (PDC, Stumpe et al. 2012; utes in Pan-STARSS I-short band on UTC 2020 March 13 from Smith et al. 2012; Stumpe et al. 2014) pipeline, producing precise the LCOGT (Brown et al. 2013) 1-m network node at Cerro Tololo Inter-American Observatory. The 4096 × 4096 LCOGT SINISTRO detrended photometry with typical precision of 150 ppm/hr for this 00 star, and then searched for exoplanetary candidates with the Tran- cameras have an image scale of 0. 389 per pixel, resulting in a 0 × 0 siting Planet Search (TPS; Jenkins et al. 2010). This identified a 26 26 field of view. The images were calibrated by the standard BANZAI strong candidate with a period of 2.54 d, a depth of only 410 ppm LCOGT pipeline (McCully et al. 2018). Photometric data AstroImageJ and a Signal to Noise Ratio (SNR) of 7.6. Automated and human were extracted using (Collins et al. 2017). The mean stellar PSF in the image sequence had a FWHM of 200. 8. Circu- vetting subsequently designated this candidate a planet candidate 00 and it was assigned TESS Object of Interest (TOI) 755.01. lar apertures with radius 3. 1 were used to extract the differential We inspected the TESS aperture using tpfplotter (plotted photometry. in Figure1; Aller et al. 2020) to ensure no nearby contaminant stars The TOI-755 SPOC pipeline transit depth of 397 ppm is too could be causing the transit. We found five stars within the aperture shallow to reliably detect with ground-based observations, so we with contrast less than 8 mag, with the brightest with a Δmag of instead checked for possible nearby eclipsing binaries (NEBs) that only 3.5. However, to cause the observed 410 ppm transit, this star could be contaminating the irregularly shaped SPOC aperture that ∼ 0 would need to host eclipses of at least 1%. Furthermore, being more generally extends 1 from the target star. To account for pos- sible contamination from the wings of neighboring star PSFs, we than 1.2 pix, and therefore almost one full-width-half-maximum 0 (FWHM) of the point-spread function (PSF), away from the target searched for NEBs out to 2. 5 from the target star. If fully blended in star, we would expect to see a significant centroid shift. However, the SPOC aperture, a neighboring star that is fainter than the target the SPOC data validation modelling (Twicken et al. 2018; Li et al. star by 8.54 magnitudes in TESS-band could produce the SPOC- 2019) shows no such shift and suggests the transit occurs within reported flux deficit at mid-transit (assuming a 100% eclipse).
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