dataesr/scientific-paragraphs-categorization huggingface dataset:
Light Curves At the time of our analysis the only TESS observations available for TOI 3714 were the Sector 19 FFI data. We made use of the QLP light curve derived from these data and available on MAST, and we used the KSPSAP detrended time series in our analysis. An ingress of TOI 3714 was observed using the MUSCAT3 instrument  (Narita et al. 2020 ) on the LCOGT 2. 0 m telescope at Haleakala on the night of 2021 September 03. Observations were gathered simultaneously through g¢, r¢, i¢, and z s filters. The data reduction and differential photometry were performed using the pipeline described in  Fukui et al. (2011). An egress was observed using MuSCAT2 on 2021 August 28 through g, i, and z s bands, while a full transit was observed with this instrument on 2021 September 25 in the g, r, i, and z s bands.
These data were reduced to light curves in a similar fashion to the MuSCAT2 observations of TOI 519. Two full transits of TOI 3714 were observed on the nights of 2022 September 21 and 2022 October 30 using the 0. 6 m TRAPPIST-North (TRAnsiting Planets and PlanetesImals Small Telescope,  Jehin et al. 2011; Gillon et al. 2011; Barkaoui et al. 2019)  telescope. The first night of observations was carried out in the I + z band, while the observations on the second night were performed using a z-band filter. Observations were scheduled using the tools of  Jensen (2013) , and the data were reduced to light curves following  Garcia et al. (2022). Two full transits of TOI 3714 were observed using the SPECULOOS-North 1. 0 m telescope  (Delrez et al. 2018; Sebastian et al. 2021; Burdanov et al. 2022 ) and an Andor ikon-L imager on the nights of 2022 October 19 and 30.
The first transit was observed in g¢, while the second was observed in r. The observations were scheduled following  Sebastian et al. (2021)  and reduced to light curves following  Murray et al. (2020)  and  Garcia et al. (2021 Garcia et al. ( , 2022)). In addition to the above transit observations, Cañas et al. (2022) also reported RBO 0. 6 m observations of TOI 3714 on the nights of 2021 August 16 and 2021 November 19 and observations with the ARCTIC imager on the ARC 3. 5 m telescope at Apache Point Observatory on the night of 2021 November 21. These data have not been published in an electronically accessible form, and we do not include them in our analysis of the system. January 01. We included these published RVs in the reanalysis of the system presented in Section 3.
High-contrast Imaging High-contrast speckle imaging was performed with the Zorro instrument on the Gemini 8 m telescope  (Scott et al. 2021). Observations were obtained at 832 and 562 nm on 2023 April 24. The data were processed following the methods of  Howell et al. (2011). No companions were detected, and contrast limits of 5. 28 and 3. 52 mag are achieved at separations greater than 0 5 in the 832 and 562 nm filters, respectively. Furthermore, no neighbors are listed within 10″ of TOI 4201 in the Gaia DR3 catalog either.
Acknowledgments The authors thank the anonymous referee for helpful comments that have improved the quality of the paper. J. H. , G. B. , and Z. C. acknowledge funding from  NASA  grant  80NSSC22K0315. This work is based in part on observations made with the Keck I telescope at  Maunakea Observatory, Hawaii. Time on this facility was awarded through  NASA. We would like to acknowledge the following individuals who contributed to gathering the Keck I/HIRES observations presented in this paper:  I. Angelo ,  A. Polanski ,  S. Yee ,  D. Tyler ,  C. Beard ,  J. Van Zandt ,  J. Akana Murphy ,  A. Mayo ,  E. Petigura ,  L. Weiss ,  G. Gilbert ,  L. Handley ,  M. MacDougall ,  F. Dai ,  A. Householder ,  M. Rice ,  N. Saunders ,  J. Zhang ,  C. Brinkman ,  M. He ,  A. Langford ,  D. Pidhorodetska ,  J.
Lubin ,  S. Blunt ,  E. Turtelboom ,  E. Louden ,  S. Dulz , and  D. Shaw. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We acknowledge  T. Gan  for contributing to the data reduction of observations from the LCOGT facilities. This work is partly supported by  JSPS KAKENHI  grant Nos. JP17H04574 ,  JP18H05439 , and  JP21K20376  and  JST CREST  grant No. JPMJCR1761. E. P. acknowledges funding from the  Spanish Ministry of Economics and Competitiveness  through project  PID2021-125627OB-C32. E. E-B. acknowledges financial support from the  European Union  and the  State Agency of Investigation of the Spanish Ministry of Science and Innovation (MICINN)  under the grant  PRE2020-093107  of the  Pre-Doc Program  for the  Training of Doctors (FPI-SO)  through FSE funds.
This article is based on observations made with the MuSCAT2 instrument, developed by  ABC , at  Telescopio Carlos Sánchez  operated on the island of Tenerife by the  IAC  in the  Spanish Observatorio del Teide. This paper is based on observations made with the MuSCAT3 instrument, developed by the  Astrobiology Center  and under financial supports by  JSPS KAKENHI  ( JP18H05439 ) and  JST PRESTO  ( JPMJPR1775 ), at  Faulkes Telescope North  on Maui, Hawaii, operated by the  Las Cumbres Observatory. A. J. acknowledges support from  ANID-Millennium Science Initiative -ICN12_009  and from  FONDECYT  project  1210718. R. B. acknowledges support from  ANID-Millennium Science Initiative -ICN12_009  and from  FONDECYT  project  11200751. H. P. acknowledges support from the  Spanish Ministry of Science and Innovation  with the  Ramon y Cajal  fellowship No.
RYC2021-031798-I. Funding from the  University of La Laguna  and the  Spanish Ministry of Universities  is acknowledged. Based on data collected under the ExTrA project at the  ESO La Silla Paranal Observatory. ExTrA is a project of  Institut de Planétologie et d'Astrophysique de Grenoble (IPAG/CNRS/UGA) , funded by the  European Research Council  under the  ERC  grant agreement No. 337591-ExTrA. ExTrA has been supported by  Labex OSUG@ 2020  ( Investissements d'avenir -ANR10 LABX56 ), the " Programme National de Physique Stellaire" (PNPS) , and the " Programme National de Palnétologie of CNRS/INSU , cofunded by  CEA  and  CNES. We thank the  Swiss National Science Foundation (SNSF)  and  Geneva University  for their continuous support to our planet search programs. This work has in particular been carried out in the frame of the  National Centre for Competence in Research  "PlanetS" supported by the  Swiss National Science Foundation (SNSF).
Funding for the TESS mission is provided by NASA's Science Mission Directorate. K. A. C. acknowledges support from the TESS mission via subaward s3449 from MIT. This publication makes use of data products from the TRAPPIST project. TRAPPIST is funded by the Belgian National Fund for Scientific Research (F. R. S. -FNRS) under grant PDRT. 0120. 21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). E. J. is F. R. S. -FNRS Senior Research Associate. M. G. is F. R. S. -FNRS Research Director. The postdoctoral fellowship of K. B. is funded by F. R. S. -FNRS grant T. 0109. 20 and by the Francqui Foundation. The ULiege's contribution to SPECULOOS has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013; grant agreement No.
The powerful combination of TESS and ESPRESSO observations has allowed several exquisite planet characterizations (e. g. ,  Damasso et al. 2020; Lillo-Box et al. 2020a; Demangeon et al. 2021; Sozzetti et al. 2021; Barros et al. 2022; Lavie et al. 2023). In this work, we confirm and characterize the small (R p = 1. 5 R ⊕ ) and close-in (P = 7. 4 days) transiting planet TOI-244 b (recently validated in  Oddo et al. 2023 ) orbiting the bright (K = 7. 97 mag) and nearby (d = 22 pc) M 2. 5V star GJ 1018. Based on the transit signal detected from TESS data, we carried out an intensive radial velocity campaign with ESPRESSO in order to confirm its planetary nature, obtain a precise mass measurement, as well as to search for additional planets. In addition to TESS and ESPRESSO data, we used complementary spectroscopic and photometric data sets from HARPS and ASAS-SN in order to maximize the information for this system.
In Sect. 2, we describe the TESS, ESPRESSO, HARPS, and ASAS-SN observations. In Sect. 3, we present our stellar characterization based on precise photometry and the ESPRESSO spectra. In Sect. 4, we describe our analysis of photometric and spectroscopic data and present the derived planetary parameters. In Sect. 5, we discuss the results, and we conclude in Sect. 6.
TESS photometry The star GJ 1018 (TOI-244, TIC 118327550) was observed by TESS (camera #2, CCD #3) at a 2-min cadence in sector 2 (S2) from 22 August 2018 to 20 September 2018, and in S29 from 26 August 2020 to 22 September 2020, resulting in a total of 36 229 target pixel files (TPFs) spanning a temporal baseline of two years. The central time of each sector shows a short gap (∼1-2 days) due to the satellite repointing toward the Earth to downlink the data, resulting in a total duty cycle of 50 days. The observations were processed by the Science Processing Operation Center (SPOC) pipeline  (Jenkins et al. 2016)  and are publicly available in the TESS archive of the Mikulski Archive for Space Telescopes (MAST) 2. The TESS SPOC data products include simple aperture photometry (SAP) and presearch dataconditioned simple aperture photometry (PDCSAP), being the latter the SAP processed by the PDC algorithm, which corrects the photometry of instrumental systematics that are common to all stars in the same CCD  (Smith et al.
Finally, the TESS Science Office examined the light curve and additional information to designate TIC 118327550. 01 as a TESS Object of Interest (TOI-244. 01) that would benefit from follow-up observations  (Guerrero et al. 2021). We downloaded from MAST the PDCSAP light curves and removed all data points with a quality flag different from zero. As a result, we removed one data point in S2 (1359. 6474 TJD) due to an argabrightening event (bit 5, value 16). In sector S29, we removed 3005 data points (located between 2098. 7624  TJD and 2101. 3791 TJD, and between 2112. 6041 TJD and 2114. We computed the generalized Lomb-Scargle periodogram (GLS; Zechmeister & Kürster 2009) of the TESS light curve (for S2 and S29 separately and jointly) and found no significant periodicities. We also computed the transit least squares periodogram (TLS;  Hippke & Heller 2019)  in order to unveil the significance of the TOI-244.
01 signal and to determine whether there are additional transit signals. To do so, we first produced a flattened version of the PDCSAP light curve in order to mitigate possible trends caused by the stellar activity or uncorrected systematics. For that matter, we filtered the photometric data of each sector separately using the robust time-windowed biweight method implemented within the wotan package  (Hippke et al. 2019 ) with a 0. 5-day window length. We detrended the PDC-SAP and joined the two flattened light curves to create a long time series. We present the detrended light curve in  Table A. 1. In Fig. 2 (left panel) , we plot the TLS periodogram of the flattened light curve, which shows a strong peak at 7. 4 days with a signal detection efficiency (SDE) of 36. 6. In the right panel, we plot the periodogram over the same light curve with the TOI-244.
Stellar atmospheric parameters We computed the stellar atmospheric parameters of GJ 1018 by means of the STEPARSYN code 8  (Tabernero et al. 2022). The code implements the spectral synthesis method with an MCMC sampler to retrieve the stellar atmospheric parameters. We employed a grid of synthetic spectra computed with the TUR-BOSPECTRUM code  (Plez 2012 ) alongside BT-Settl stellar atmospheric models  (Allard et al. 2012 ) and atomic and molecular data of the Vienna atomic line database (VALD3;  Ryabchikova et al. 2015). We considered a selection of Fe I, Ti I lines, and TiO molecular bands that are well-suited to analyze M-dwarf stars  (Marfil et al. 2021). In all, STEPARSYN has allowed us to compute the following stellar parameters: T eff = 3433 ± 10 K, log g = 4. 66 ± 0. 07 dex, and [Fe/H] = -0.
Although ODUSSEAS was initially developed for spectra with resolution powers from 48 000 to 115 000, it has been applied successfully to ESPRESSO spectra with a resolution power of 140 000. For the very high resolutions of ESPRESSO and HARPS, the results derived by ODUSSEAS are essentially the same either by using directly the original highest-resolution spectra of ESPRESSO, or by convolving first the ESPRESSO spectra to the lower, but still high, resolution of HARPS. We ran ODUSSEAS by considering a reference data set composed of 47 stars with interferometry-based T eff  (Rabus et al. 2019; Khata et al. 2021) , and [Fe/H] derived through the photometric calibration by  Neves et al. (2012)  using the Gaia DR3 parallaxes. We obtain T eff = 3419 ± 92 K and [Fe/H] = -0. 03 ± 0. 11 dex. The ODUSSEAS effective temperature is in very good agreement with the value computed by STEPARSYN.
Stellar bolometric luminosity To determine the bolometric luminosity of GJ 1018, we first built the photometric spectral energy distribution (SED) of the star using broadband and narrowband photometry from the literature. The stellar SED is shown in Fig. 5 , which includes the Galaxy Evolution Explorer (GALEX) near-ultraviolet photometry  (Bianchi et al. 2017) , the Johnson BVRI photometry  (Ducati 2002) , the BV data from the AAVSO Photometric All-sky Survey (APASS; Henden 2019), the griz data from the Sloan Digital Sky Survey  (York et al. 2000) , the Gaia Early Data Release 3 photometry (Gaia Collaboration 2021), the y data from the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS;  Flewelling et al. 2020 ), the Two Micron All Sky Survey (2MASS) near-infrared JHK s photometry  (Skrutskie et al.
2006) , the Wide-field Infrared Survey Explorer (WISE) W1, W2, W3, and W4 data  (Wright et al. 2010) , and the optical multiphotometry of the Observatorio Astrofísico de Javalambre (OAJ) Physics of the Accelerating Universe Astrophysical Survey (JPAS) and Photometric Local Universe Survey (JPLUS) catalogs accessible through the Spanish Virtual Observatory  (Bayo et al. 2008). In total, there are 89 photometric data points defining the SED of GJ 1018 between 0. 23 and ∼25 µm. The OAJ/JPAS data cover very nicely the optical region in the interval 0. 40-0. 95 µm with a cadence of one measurement per 0. 01 µm. We used the Gaia trigonometric parallax to convert all observed photometry and fluxes into absolute fluxes, which we present in Table  A. 5. The SED of GJ 1018 clearly indicates its photospheric origin for wavelengths longer than 0.
The first run (or burn-in) consisted of 200 000 iterations. After this run, we reset the sampler and initialized the second run (or production) with 100 000 iterations while considering the initial values from the last iteration of the burn-in phase. To ensure the convergence of the chains, we estimated the autocorrelation time for each parameter and checked that it is at least 30 times smaller than the chain length. We ran an MCMC fit starting from wide uniform priors for all the parameters involved in the model except for those for which we have prior information, which we constrained through Gaussian priors. These parameters are the T 0 and P of TOI-244. 01 (from the TLS periodogram, Sect. 2. 1), the stellar radius and mass (from our spectroscopic analysis, Sect. 3. 4), and the quadratic LD coefficients, which we computed from the ldtk package  (Parviainen & Aigrain 2015).
The package infers the coefficients of a given LD law relying on the  Husser et al. (2013)  synthetic spectra library, spectroscopic T eff , log g, and [Fe/H], and the instrument transmission curve. We used the ldtk uncertainties as the widths of the Gaussian distributions. In order to account for possible systematics in the estimated LD coefficients (e. g. ,  Patel & Espinoza 2022) , we also ran the MCMC fit by considering conservative widths of 0. 2, obtaining identical results for the planetary parameters. We show the prior distributions for this analysis and subsequent ones in Table  3. In Table  A. 6, we include the median and 1σ (68. 3% credible intervals) of the posterior distributions of the fit parameters. In Fig. 6 , we show the complete TESS light curve together with the global model (transit + GP) evaluated on the fit parameters.
ESPRESSO and HARPS radial velocity analysis We analyzed the ESPRESSO and HARPS RV data sets described in Sects. 2. 2 and 2. 3 through a model composed of three components: a Keplerian, which models planetary-induced RV signals, an instrumental component, which models the systemic velocity as measured by each instrument, and a GP, which models the RV correlated noise induced by the stellar activity. We implemented the Keplerian component through the Python package radvel  (Fulton et al. 2018 ) by using the parametrization P, T 0 , K, √ e cos(w), √ e sin(w) , being P the orbital period of the planet, T 0 the time of inferior conjunction, K the semi-amplitude, e the orbital eccentricity, and w the planetary argument of periastron. The instrumental component of our model consists of an offset that corresponds to the systemic radial velocity of the star as measured by each instrument (γ ins ).
instrument (σ ins ) that we added quadratically to the uncertainties of our RV measurements. In order to obtain a more robust estimation of the model parameters, we included to our data set an activity indicator to be modeled jointly with the HARPS and ESPRESSO RVs. This approach consists of using two GP kernels with shared hyperparameters except the signal amplitude (hereafter we differentiate between η 1,RV and η 1,indicator ). This approach has been used in previous works and relies on the assumption that the variations on the activity indicators are caused by the stellar activity alone, and that their periodicity and coherence are the same as those of the activity component of the RV (e. g. , Suárez  Mascareño et al. 2020; Lillo-Box et al. 2020a; Barros et al. 2022). From the time series and periodograms of Fig.
2016 (Zeng et al. , 2019)). Right: color coding indicates the stellar insolation received by the planets. The dashed lines correspond to theoretical models from  Zeng et al. (2019) , which consider planets without a significant amount of volatiles (back and red lines), planets with condensed water (dark blue), and planets with H 2 atmospheric envelopes (light blue). The dotted lines correspond to the  Turbet et al. (2020)  theoretical models for Earth-like planets with H 2 O-dominated atmospheres. These plots have been prepared using mr-plotter, which is available at https://github. com/castro-gzlz/mr-plotter/. Seager et al. 2007; Swift et al. 2012; Zeng et al. 2016). In recent work,  Turbet et al. (2020)  computed new mass-radius relationships taking into account that for H 2 O-rich rocky planets more irradiated than the runaway greenhouse limit (i.
Acknowledgements. We thank the anonymous referee for the thorough report and quick response. A. C. -G. is funded by the  Spanish Ministry of Science  through  MCIN/AEI/10. 13039/501100011033  grant  PID2019-107061GB-C61. J. L. -B. is supported by the  Spanish Ministry of Science  through the  Ramón y Cajal program  with code  RYC2021-031640-I  (funded through  MCIN/AEI/10. 13039/501100011033  and the  NextGenerationEU/PRTR  from the  European Union)  and the  "la Caixa" Foundation  ( ID 100010434 ) and from the  European Unions   Horizon 2020 research and innovation programme  under the  Marie Sklodowska-Curie  grant agreement No  847648 , with fellowship code  LCF/BQ/PI20/11760023. Y. A. and J. D. acknowledge the support of the  Swiss National Foundation  though grant  192038. This work has been carried out within the framework of the NCCR PlanetS supported by the  Swiss National Science Foundation  under grants  51NF40_182901  and  51NF40_205606.
J. I. G. H. , C. A. P. , and A. S. M. acknowledge financial support from the  Spanish Ministry of Science and Innovation (MICINN)  project  PID2020-117493GB-I00. C. A. P. is also thankful for funding from the  Spanish government  through grants  AYA2014-56359-P  and  AYA2017-86389-P. A. S. M. and J. I. G. H. also acknowledge financial support from the  Government of the Canary Islands  project  ProID2020010129. This material is based upon work supported by  NASA's Interdisciplinary Consortia for Astrobiology Research  ( NNH19ZDA001N- ICAR ) under award number  19-ICAR19_2-0041. This work was supported by  FCT -Fundação para a Ciência e a Tecnologia  through national funds and by  FEDER  through  COMPETE2020 -Programa Operacional Competitividade e Internacionalização  by these grants:  UIDB/04434/2020 ;  UIDP/04434/2020 ;  2022.
This publication makes use of VOSA, developed under the  Spanish Virtual Observatory  (https://svo. cab. inta-csic. es) project funded by  MCIN/AEI/10. 13039/501100011033/  through grant  PID2020-112949GB-I00. This work made use of tpfplotter by  J. Lillo-Box  (publicly available in www. github. com/jlillo/tpfplotter), which also made use of the python packages astropy, lightkurve, matplotlib and numpy. This work has made use of data from the  European Space Agency (ESA)  mission Gaia (https://www. cosmos. esa. int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www. cosmos. esa. int/web/ gaia/dpac/consortium). We acknowledge the use of public TESS data from pipelines at the  TESS Science Office  and at the  TESS Science Processing Operations Center. Resources  supporting this work were provided by the  NASA High-End Computing (HEC)   Program  through the  NASA Advanced Supercomputing (NAS) Division at Ames Research Center  for the production of the SPOC data products.
This research has made use of the Exoplanet Follow-up  Observation Program  (ExoFOP; DOI: 10. 26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of the NASA Exoplanet Archive,which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of the SIMBAD database (Wenger et al. 2000), operated at CDS, Strasbourg, France. This work has made use of the following software: astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), numpy (Harris et al. 2020), scipy (Virtanen et al. 2020), and lightkurve (Lightkurve Collaboration 2018).
8 Fig. 5. Photometric spectral energy distribution of GJ 1018 from 0. 23 to ∼25 µm. The PHOENIX model corresponding to 3300 K, solar metallicity and high gravity is added (Allard et al. 2003) in order to show that most fluxes are photospheric in origin and that there is no infrared flux excesses at long wavelengths. Vertical error bars denote flux uncertainties and horizontal error bars account for the width of the passbands. The fluxes, effective wavelengths and widths of all passbands were taken from the Virtual Observatory SED Analyzer database.
Observations The Fermi-GBM triggered on GRB 220101A at 05:10:11. 51 UT on January 1, 2022  [1]. The burst was also detected by the Fermi-LAT at high energies  [2]. The LAT on-ground localization of the event is RA, Dec = 1. 52 • , 31. 75 • with an error radius of 0. 46 •. GRB 220101A is the most-distant LAT-detected burst to date with a redshift 𝑧 = 4. 618  [3]. In this work we used the GBM Time Tagged Events (TTE) recorded by the NaI detectors 3, 6, 7, 9, and by the BGO detector 1. We used the LAT standard P8R3_TRANSIENT020E_V2 data, and additionally the LAT Low Energy (LLE  [4] ) data to extend our analysis down to 20 MeV. Figure  1  shows the Fermi multi-detector light curve of GRB 220101A during its prompt emission (𝑇 90 ∼ 128 s  [1] ). Interestingly, the high-energy flux is attenuated above ∼ 100 MeV during the brightest emission episode around 𝑇 0 + 100 s (time bins B and C).