Search

Your search keyword '"Subjak, J."' showing total 6 results
Start Over Author "Subjak, J." Publication Year Range Last 3 years
6 results on '"Subjak, J."'

1. Five new eclipsing binaries with low-mass companions

Author

Lipták, J., Skarka, M., Guenther, E., Chaturvedi, P., Vítková, M., Karjalainen, R., Šubjak, J., Hatzes, A., Bieryla, A., Gandolfi, D., Albrecht, S. H., Beck, P. G., Deeg, H. J., Everett, M. E., Higuera, J., Jones, D., Mathur, S., Patel, Y. G., Persson, C. M., Redfield, S., and Kabáth, P.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Precise space-based photometry from the Transiting Exoplanet Survey Satellite results in a huge number of exoplanetary candidates. However, the masses of these objects are unknown and must be determined by ground-based spectroscopic follow-up observations, frequently revealing the companions to be low-mass stars rather than exoplanets. We present the first orbital and stellar parameter solutions for five such eclipsing binary-star systems using radial-velocity follow-up measurements together with spectral-energy-distribution solutions. TOI-416 and TOI-1143 are totally eclipsing F+M star systems with well-determined secondary masses, radii, and temperatures. TOI-416 is a circular system with an F6 primary and a secondary with a mass of $M_2={0.131(8)}{M_\odot}$. TOI-1143 consists of an F6 primary with an $M_2={0.142(3)}{M_\odot}$ secondary on an eccentric orbit with a third companion. With respect to the other systems, TOI-1153 shows ellipsoidal variations, TOI-1615 contains a pulsating primary, and TOI-1788 has a spotted primary, while all have moderate mass ratios of 0.2-0.4. However, these systems are in a grazing configuration, which limits their full description. The parameters of TOI-416B and TOI-1143B are suitable for the calibration of the radius-mass relation for dwarf stars., Comment: A&A accepted on 06/06/2024

Published
2024
Full Text
View/download PDF

2. TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet

Author

Korth, J., Gandolfi, D., Šubjak, J., Howard, S., Ataiee, S., Collins, K. A., Quinn, S. N., Mustill, A. J., Guillot, T., Lodieu, N., Smith, A. M. S., Esposito, M., Rodler, F., Muresan, A., Abe, L., Albrecht, S. H., Alqasim, A., Barkaoui, K., Beck, P. G., Burke, C. J., Butler, R. P., Conti, D. M., Collins, K. I., Crane, J. D., Dai, F., Deeg, H. J., Evans, P., Grziwa, S., Hatzes, A. P., Hirano, T., Horne, K., Huang, C. X., Jenkins, J. M., Kabáth, P., Kielkopf, J. F., Knudstrup, E., Latham, D. W., Livingston, J., Luque, R., Mathur, S., Murgas, F., Osborne, H. L. M., Pallé, E., Persson, C. M., Rodriguez, J. E., Rose, M., Rowden, P., Schwarz, R. P., Seager, S., Serrano, L. M., Sha, L., Shectman, S. A., Shporer, A., Srdoc, G., Stockdale, C., Tan, T. G., Teske, J. K., Van Eylen, V., Vanderburg, A., Vanderspek, R., Wang, S. X., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c, on an 8.4-day orbit, accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We perform a photodynamical modeling of the HARPS and PFS RVs, and transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program. We determine the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 $\pm$ 0.97 M$_\oplus$ and Rb = 3.56 $\pm$ 0.13 R$_\oplus$, and Mc = 325.59 $\pm$ 5.59 M$_\oplus$ and Rc = 13.32+1.55-1.41 R$_\oplus$, respectively. We spectroscopically confirm TOI-1130 b that was previously only validated. We find that the two planets orbit with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small yet increasing population of hot Jupiters with an inner low-mass planet that challenges the pathway for hot Jupiter formation. We also detect a linear RV trend possibly due to the presence of an outer massive companion., Comment: 19 pages, Accepted to A&A

Published
2023
Full Text
View/download PDF

3. Search for planets around stars with wide brown dwarfs

Author

Šubjak, J., Lodieu, N., Kabáth, P., Boffin, H. M. J., Nowak, G., Grundahl, F., Béjar, V. J. S., Osorio, M. R. Zapatero, and Antoci, V.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. The project aims to understand better the role of wide brown dwarf companions on planetary systems. Methods. We obtained high-resolution spectra of six bright stars with co-moving wide substellar companions with the SONG, CARMENES, and STELLA high-resolution spectrographs. We used these spectra to derive radial velocities together with a complete set of stellar physical parameters. We then investigated radial velocities signals and discussed the fraction of planets in such systems. We also re-analyzed the ages of our targets, which were used to derive the physical parameters of wide brown dwarf companions. Finally, a compilation of systems with known planets from the literature is considered along with our sample to search for possible peculiarities in their parameter distributions. Results. Based on the derived ages of six observed systems, we re-computed the masses of the wide companions, confirming their substellar nature. We confirmed planets in the HD 3651 and HIP 70849 systems and found a new planetary candidate in the HD 46588 system. In our survey, which is sensitive mostly to Neptune-mass planets at short periods of a few days and Saturn-mass planets at longer periods of hundreds of days, we derived a frequency of planets orbiting stars with wide brown dwarf companions below 70% with the uncertainties included. Comparing the parameter distributions of our sample with single stars, we observe the enhancement of planets with short periods below six days in systems with a wide stellar companion. Finally, planets in systems with wide BD companions follow their own eccentricity distribution with a maximum at $\sim0.65$ and have periods larger than 40 days, masses larger than $0.1\,M_J$, and eccentricities larger than 0.4., Comment: 28 pages, 31 figures, accepted for publication in Astronomy & Astrophysics

Published
2022
Full Text
View/download PDF

4. TOI-1268b: the youngest, hot, Saturn-mass transiting exoplanet

Author

Šubjak, J., Endl, M., Chaturvedi, P., Karjalainen, R., Cochran, W. D., Esposito, M., Gandolfi, D., Lam, K. W. F., Stassun, K., Žák, J., Lodieu, N., Boffin, H. M. J., MacQueen, P. J., Hatzes, A., Guenther, E. W., Georgieva, I., Grziwa, S., Schmerling, H., Skarka, M., Blažek, M., Karjalainen, M., Špoková, M., Isaacson, H., Howard, A. W., Burke, C. J., Van Eylen, V., Falk, B., Fridlund, M., Goffo, E., Jenkins, J. M., Korth, J., Lissauer, J. J., Livingston, J. H., Luque, R., Muresan, A., Osborn, H. P., Pallé, E., Persson, C. M., Redfield, S., Ricker, G. R., Seager, S., Serrano, L. M., Smith, A. M. S., and Kabáth, P.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of TOI-1268b, a transiting Saturn-mass planet from the TESS space mission. With an age of less than one Gyr, derived from various age indicators, TOI-1268b is the youngest Saturn-mass planet known to date and contributes to the small sample of well characterised young planets. It has an orbital period of $P\,=\,8.1577080\pm0.0000044$ days, and transits an early K dwarf star with a mass of $M_\star$ = $ 0.96 \pm 0.04$ $M_{\odot}$, a radius of $R_\star$ = $ 0.92 \pm 0.06$ $R_{\odot}$, an effective temperature of $T_\mathrm{eff}\,=\,5300\pm100$ K, and a metallicity of $0.36\pm0.06$ dex. By combining TESS photometry with high-resolution spectra acquired with the Tull spectrograph at McDonald observatory, and the high-resolution spectrographs at Tautenburg and Ondrejov observatories, we measured a planetary mass of $M_\mathrm{p}\,=\,96.4 \pm 8.3\,M_{\oplus}$ and a radius of $R_\mathrm{p}\,=\,9.1 \pm 0.6\,R_{\oplus}$. TOI-1268 is an ideal system to study the role of star-planet tidal interactions for non-inflated Saturn-mass planets. We used system parameters derived in this paper to constrain the planet tidal quality factor to the range of $10^{4.5-5.3}$. When compared with the sample of other non-inflated Saturn-mass planets, TOI-1268b is one of the best candidates for transmission spectroscopy studies., Comment: 21 pages, 17 figures, accepted for publication in Astronomy & Astrophysics; see independent work by Dong et al. for Rossiter-McLaughlin measurement of TOI-1268b

Published
2022
Full Text
View/download PDF

5. TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Subjak, J, Endl, M, Chaturvedi, P, Karjalainen, R, Cochran, WD, Esposito, M, Gandolfi, D, Lam, KWF, Stassun, K, Zák, J, Lodieu, N, Boffin, HMJ, MacQueen, PJ, Hatzes, A, Guenther, EW, Georgieva, I, Grziwa, S, Schmerling, H, Skarka, M, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Subjak, J, Endl, M, Chaturvedi, P, Karjalainen, R, Cochran, WD, Esposito, M, Gandolfi, D, Lam, KWF, Stassun, K, Zák, J, Lodieu, N, Boffin, HMJ, MacQueen, PJ, Hatzes, A, Guenther, EW, Georgieva, I, Grziwa, S, Schmerling, H, and Skarka, M

Abstract

We report the discovery of TOI-1268b, a transiting Saturn-mass planet from the TESS space mission. With an age of less than 1 Gyr, derived from various age indicators, TOI-1268b is the youngest Saturn-mass planet known to date; it contributes to the small sample of well-characterised young planets. It has an orbital period of P = 8.1577080 ± 0.0000044 days, and transits an early K-dwarf star with a mass of M? = 0.96 ± 0.04 M , a radius of R? = 0.92 ± 0.06 R , an effective temperature of Teff = 5300 ± 100 K, and a metallicity of 0.36 ± 0.06 dex. By combining TESS photometry with high-resolution spectra acquired with the Tull spectrograph at the McDonald Observatory, and the high-resolution spectrographs at the Tautenburg and Ondˇrejov Observatories, we measured a planetary mass of Mp = 96.4 ± 8.3 M⊕ and a radius of Rp = 9.1 ± 0.6 R⊕. TOI-1268 is an ideal system for studying the role of star-planet tidal interactions for non-inflated Saturn-mass planets. We used system parameters derived in this paper to constrain the planet’s tidal quality factor to the range of 104.5−5.3 . When compared with the sample of other non-inflated Saturn-mass planets, TOI-1268b is one of the best candidates for transmission spectroscopy studies.

Published
2023

6. TOI-2046b, TOI-1181b, and TOI-1516b, three new hot Jupiters from TESS: planets orbiting a young star, a subgiant, and a normal star

Author

Kabath, P., Chaturvedi, P., MacQueen, P., Skarka, M., Subjak, J., Esposito, M., Cochran, W. D., Bellomo, Salvatore E., Karjalainen, Raine, Guenther, E. W., Endl, M, Csizmadia, Szilard, Karjalainen, Marie, Hatzes, A. P., Zak, J, Gandolfi, D., Boffin, H. M. J., Vines, J. I, Livingston, J., Garcia, Rafael A., Mathur, S., Gonzalez-Cuesta, Lucia, Blazek, M., Caldwell, Douglas A., Colón, Knicole D., Deeg, H, Erikson, A, Van Eylen, Vincent, Fong, William, Fridlund, M., Fukui, A., Furesz, G, Goeke, R.F., Goffo, E., Howell, S.B., Jenkins, J.M., Klagyivik, Peter, Korth, J., Latham, David W., Luque, R., Moldovan, Dan, Murgas, F., Narita, N., Orell-Miquel, J., Palle, E., Parviainen, H, Persson, C., Reed, Phillip. A., Redfield, Seth, Ricker, George R., Seager, S., Serrano, L. M., Shporer, A., Smith, Alexis M S, Watanabe, N., Winn, J. N., Kesprint, Team, Ministerio de Ciencia e Innovación (España), and European Commission

Subjects
stars, planets and satellites: detection, FOS: Physical sciences, techniques spectroscopic, Astrophysics::Cosmology and Extragalactic Astrophysics, TOI-2046, spectroscopic [Techniques], Stars: individual: TOI-1181, TOI-1516, TOI-2046, TOI-1516, techniques radial velocities, techniques: radial velocities, Astrophysics::Solar and Stellar Astrophysics, individual, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, individual: TOI-1181, TOI-1516, TOI-2046 [Stars], Earth and Planetary Astrophysics (astro-ph.EP), TOI-1181, radial velocities [Techniques], Astronomy and Astrophysics, detection [Planets and satellites], planets and satellites detection, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: individual: TOI-1181, Astrophysics::Earth and Planetary Astrophysics, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract

Full list of authors: Kabath, Petr; Chaturvedi, Priyanka; MacQueen, Phillip J.; Skarka, Marek; Subjak, Jan; Esposito, Massimilliano; Cochran, William D.; Bellomo, Salvatore E.; Karjalainen, Raine; Guenther, Eike W.; Endl, Michael; Csizmadia, Szilard; Karjalainen, Marie; Hatzes, Artie; Zak, Jiri; Gandolfi, Davide; Boffin, Henri M. J.; Vines, Jose, I; Livingston, John H.; Garcia, Rafael A.; Mathur, Savita; Gonzalez-Cuesta, Lucia; Blazek, Martin; Caldwell, Douglas A.; Colon, Knicole D.; Deeg, Hans; Erikson, Anders; Van Eylen, Vincent; Fong, William; Fridlund, Malcolm; Fukui, Akihiko; Furesz, Gabor; Goeke, Robert F.; Goffo, Elisa; Howell, Steve; Jenkins, Jon M.; Klagyivik, Peter; Korth, Judith; Latham, David W.; Luque, Rafael; Moldovan, Dan; Murgas, Felipe; Narita, Norio; Orell-Miquel, Jaume; Palle, Enric; Parviainen, Hannu; Persson, Carina M.; Reed, Phillip A.; Redfield, Seth; Ricker, George R.; Seager, Sara; Serrano, Luisa Maria; Shporer, Avi; Smith, Alexis M. S.; Watanabe, Noriharu; Winn, Joshua N.; KESPRINT Team., We present the confirmation and characterization of three hot Jupiters, TOI-1181b, TOI-1516b, and TOI-2046b, discovered by the TESS space mission. The reported hot Jupiters have orbital periods between 1.4 and 2.05 d. The masses of the three planets are 1.18 ± 0.14 MJ, 3.16 ± 0.12 MJ, and 2.30 ± 0.28 MJ, for TOI-1181b, TOI-1516b, and TOI-2046b, respectively. The stellar host of TOI-1181b is a F9IV star, whereas TOI-1516b and TOI-2046b orbit F main sequence host stars. The ages of the first two systems are in the range of 2–5 Gyrs. However, TOI-2046 is among the few youngest known planetary systems hosting a hot Jupiter, with an age estimate of 100–400 Myrs. The main instruments used for the radial velocity follow-up of these three planets are located at Ondřejov, Tautenburg, and McDonald Observatory, and all three are mounted on 2–3 m aperture telescopes, demonstrating that mid-aperture telescope networks can play a substantial role in the follow-up of gas giants discovered by TESS and in the future by PLATO. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society, This work is done under the framework of the KESPRINT collaboration (http://www.kesprint.science). KESPRINT is an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions. This work is based on data sets obtained with the Perek 2-m telescope. PK, JS, MS, RK, and MB are acknowledging the support by Inter-transfer grant no LTT-20015. MK acknowledges the support from ESA-PRODEX PEA4000127913. PK and JS acknowledge a travel budget from ERASMUS + grant 2020-1-CZ01-KA203-078200. HB’s mobility was funded under: MŠMT – CZ.02.2.69/0.0/0.0/18_053/0016972 Podpora mezinárodní spolupráce v astronomii. PC acknowledges the generous support from Deutsche Forschungsgemeinschaft (DFG) of the grant CH 2636/1-1. PR acknowledges support from National Science Foundations (NSF) grant No. 1952545. This work was generously supported by the Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. 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. JIV acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This work is partly supported by JSPS KAKENHI Grant Number JP20K14518. JK gratefully acknowledge the support of the Swedish National Space Agency (SNSA; DNR 2020-00104). HD acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant PID2019-107061GB-C66, DOI: 10.13039/501100011033. RL acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence ’Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). 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). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This is University of Texas Center for Planetary Systems Habitability contribution #0054. LGC acknowledges support from grant FPI-SO from the Spanish Ministry of Economy and Competitiveness (MINECO) (research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610). SM acknowledges support by the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697 and the grant number PID2019-107187GB-I00. RAG acknowledges the support from PLATO and GOLF CNES grants. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Observations in the paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. The authors are honored to be permitted to conduct observations on Iolkam Du’ag (Kitt Peak), a mountain within the Tohono O’odham Nation with particular significance to the Tohono O’odham people. This work is partly supported by JSPS KAKENHI Grant Number JP17H04574 and JP18H05439, JST PRESTO Grant Number JPMJPR1775, the Astrobiology Center of National Institutes of Natural Sciences (NINS; Grant Number AB031010). 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. Observations in the paper made use of the High-Resolution Imaging instrument ‘Alopeke. ‘Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).

Published
2022

Catalog

Books, media, physical & digital resources
See catalog results