@article{MTMT:34554832,
	title = {Correcting Exoplanet Transmission Spectra for Stellar Activity with an Optimized Retrieval Framework},
	url = {https://m2.mtmt.hu/api/publication/34554832},
	author = {Thompson, Alexandra and Biagini, Alfredo and Cracchiolo, Gianluca and Petralia, Antonino and Changeat, Quentin and Saba, Arianna and Morello, Giuseppe and Morvan, Mario and Micela, Giuseppina and Tinetti, Giovanna},
	doi = {10.3847/1538-4357/ad0369},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {960},
	unique-id = {34554832},
	issn = {1538-4357},
	abstract = {The chromatic contamination that arises from photospheric heterogeneities, e.g., spots and faculae on the host star presents a significant noise source for exoplanet transmission spectra. If this contamination is not corrected for, it can introduce substantial bias in our analysis of the planetary atmosphere. We utilize two stellar models of differing complexity, StARPA (Stellar Activity Removal for Planetary Atmospheres) and ASteRA (Active Stellar Retrieval Algorithm), to explore the biases introduced by stellar contamination in retrieval under differing degrees of stellar activity. We use the retrieval framework TauREx3 and a grid of 27 synthetic, spot-contaminated transmission spectra to investigate potential biases and to determine how complex our stellar models must be in order to accurately extract the planetary parameters from transmission spectra. The input observation is generated using the more complex model (StARPA), in which the spot latitude is an additional, fixable parameter. This observation is then fed into a combined stellar-planetary retrieval, which contains a simplified stellar model (ASteRA). Our results confirm that the inclusion of stellar activity parameters in retrieval minimizes bias under all activity regimes considered. ASteRA performs very well under low-to-moderate activity conditions, retrieving the planetary parameters with a high degree of accuracy. For the most active cases, characterized by larger, higher-temperature contrast spots, some minor residual bias remains due to ASteRA neglecting the interplay between the spot and the limb-darkening effect. As a result of this, we find larger errors in retrieved planetary parameters for central spots (0°) and those found close to the limb (60°) than those at intermediate latitudes (30°).},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; EXOPLANETS; Astrophysics - Earth and Planetary Astrophysics; Stellar Activity; Exoplanet Atmospheres; Transmission spectroscopy; 498; 487; 1580; 2133},
	year = {2024},
	eissn = {0004-637X},
	pages = {107}
}

@article{MTMT:34554831,
	title = {To Sample or Not to Sample: Retrieving Exoplanetary Spectra with Variational Inference and Normalizing Flows},
	url = {https://m2.mtmt.hu/api/publication/34554831},
	author = {Yip, Kai Hou and Changeat, Quentin and Al-Refaie, Ahmed and Waldmann, Ingo P.},
	doi = {10.3847/1538-4357/ad063f},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {961},
	unique-id = {34554831},
	issn = {1538-4357},
	abstract = {Current endeavours in exoplanet characterization rely on atmospheric retrieval to quantify crucial physical properties of remote exoplanets from observations. However, the scalability and efficiency of said technique are under strain with increasing spectroscopic resolution and forward model complexity. The situation has become more acute with the recent launch of the James Webb Space Telescope and other upcoming missions. Recent advances in machine learning provide optimization-based variational inference as an alternative approach to perform approximate Bayesian posterior inference. In this investigation we developed a normalizing-flow-based neural network, combined with our newly developed differentiable forward model, Diff-τ, to perform Bayesian inference in the context of atmospheric retrievals. Using examples from real and simulated spectroscopic data, we demonstrate the advantages of our proposed framework: (1) training our neural network does not require a large precomputed training set and can be trained with only a single observation; (2) it produces high-fidelity posterior distributions in excellent agreement with sampling-based retrievals; (3) it requires up to 75% fewer forward model calls to converge to the same result; and (4) this approach allows formal Bayesian model selection. We discuss the computational efficiencies of Diff-τ in relation to TauREx3's nominal forward model and provide a "lessons learned" account of developing radiative transfer models in differentiable languages. Our proposed framework contributes toward the latest development of neural network-powered atmospheric retrieval. Its flexibility and significant reduction in forward model calls required for convergence holds the potential to be an important addition to the retrieval tool box for large and complex data sets along with sampling-based approaches.},
	keywords = {NEURAL NETWORKS; Bayesian statistics; EXOPLANETS; Exoplanet Atmospheres; observational astronomy; posterior distribution; Transmission spectroscopy; 498; 1145; 487; 1900; 1933; 1926; 2133},
	year = {2024},
	eissn = {0004-637X},
	pages = {30}
}

@article{MTMT:34545462,
	title = {Pulsation in TESS Objects of Interest},
	url = {https://m2.mtmt.hu/api/publication/34545462},
	author = {Gomes, R. L. and Canto, Martins B. L. and Fontinele, D. O. and Almeida, L. A. and Freire, R. Alves and Brito, A. C. and de, Amorim R. G. S. B. and Ferreira, Lopes C. E. and Hazarika, D. and Janot-Pacheco, E. and Leão, I. C. and Messias, Y. S. and Souza, R. A. A. and De, Medeiros J. R.},
	doi = {10.3847/1538-4357/ad0b0a},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {961},
	unique-id = {34545462},
	issn = {1538-4357},
	abstract = {We report the discovery of three Transiting Exoplanet Survey Satellite Objects of Interest (TOI) with signatures of pulsation, observed in more than one sector. Our main goal is to explore how large is the variety of classical pulsators such as δ Sct, γ Dor, RR Lyrae and Cepheid among TOI pulsators. The analysis reveals two stars with signatures of δ Sct and one of γ Dor, out of a sample of 3901 TOIs with available light curves (LCs). To date, there is a very scarce number of known pulsating stars hosting planets. The present finding also emerges as an exciting laboratory for studying different astrophysical phenomena, including the effects of star-planet interaction on pulsation and timing detection of planetary companions. We have also identified 16 TOI stars with periodicities and LCs morphology compatible with different classical pulsating classes, but for most of them, the dominant frequency signals originate from contaminating sources.},
	keywords = {Transit Photometry; Stellar pulsations; Substellar companion stars; 1709; 1648; 1625; 2177; Star-planet interactions},
	year = {2024},
	eissn = {0004-637X},
	pages = {55}
}

@article{MTMT:34525643,
	title = {Discovery of Two Different Full Disk Evolutionary Patterns of M-type T Tauri Stars with LAMOST DR8},
	url = {https://m2.mtmt.hu/api/publication/34525643},
	author = {Haerken, Hasitieer and Li, Guang-Wei and Li, Min and Duan, Fuqing and Zhao, Yongheng},
	doi = {10.3847/1538-4357/ad04d3},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {960},
	unique-id = {34525643},
	issn = {1538-4357},
	abstract = {The full disk, full of gas and dust, determines the upper limit of planet masses, and its lifetime is critical for planet formation, especially for giant planets. In this work, we studied the evolutionary timescales of the full disks of T Tauri stars (TTSs) and their relations to accretion. Combined with Gaia EDR3, Two Micron All Sky Survey, and Wide-field Infrared Survey Explorer data, 1077 disk-bearing TTS candidates were found in LAMOST DR8, and stellar parameters were obtained. Among them, 783 are newly classified by spectra as classical T Tauri stars (CTTSs; 169) or weak-lined T Tauri stars (WTTSs). Based on EW and FWHM of Hα, 157 TTSs in accretion were identified, with ~82% also having full disks. For TTSs with M < 0.35M ☉, about 80% seem to already lose their full disks at ~0.1 Myr, which may explain their lower mass, while the remaining 20% with full disks evolve at similar rates of non-full disks within 5 Myr, allowing enough time and material to form giant planets. The fraction of accreting TTSs to disk-bearing TTSs is stable at ~10% and can last ~5-10 Myr, suggesting that full disks and accretion evolve with similar rates as non-full disks. For TTSs with M > 0.35 M ☉, almost all full disks can survive more than 0.1 Myr, most for 1 Myr and some even for 20 Myr. For TTSs with M > 0.35 M ☉, almost all full disks can survive more than 0.1 Myr, most for 1 Myr, and some even for 20 Myr, which implies planets are more likely to be formed in their disks than those of M < 0.35 M ☉, and thus M dwarfs with M > 0.35 M ☉ can have more planets. The fraction of full-disk TTSs to disk-bearing TTSs decreases with age following the relation f ∝ t -0.35, and similar relations existed in the fraction of accreting TTSs and the fraction of full-disk CTTSs, suggesting faster full disks and accretion evolution than non-full disks. For full-disk stars, the ratio of accretion of lower-mass stars is systematically lower than that of higher-mass stars, confirming the dependence of accretion on stellar mass, which may be reflective of an observational bias in the detection of accretion levels, with the lower-mass stars crossing below the detection threshold earlier than higher-mass stars.},
	keywords = {ACCRETION; Astrophysics - Solar and Stellar Astrophysics; T TAURI STARS; CIRCUMSTELLAR DISKS; Astrophysics - Earth and Planetary Astrophysics; 14; 1681; 235},
	year = {2024},
	eissn = {0004-637X},
	pages = {58}
}

@article{MTMT:34517330,
	title = {4FGL J1318.2+6754: A Long Orbital-period Redback Candidate},
	url = {https://m2.mtmt.hu/api/publication/34517330},
	author = {Lin, Jie and Chen, Hailiang and Wang, Bojun and Xu, Renxin},
	doi = {10.3847/2041-8213/ad1580},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {960},
	unique-id = {34517330},
	issn = {1538-4357},
	abstract = {By combining the Fermi catalog and the single-lined spectroscopic binaries of Gaia Data Release 3 (DR3), we report a new candidate redback millisecond pulsar binary, which is recommended as a target for radio telescopes to detect pulsed signals. Using TESS data in the T band spanning over 4 yr, we find a period of ~4.13 days, which is consistent with the radial velocity solution of the Gaia DR3 and optical spectroscopy from the LAMOST telescope. The light curve in the T band reveals periodic modulation of low amplitude that is a characteristic feature of the heating of the photosphere of a nondegenerate low-mass stellar companion by the pulsar wind. The nondegenerate companion is a bright (G = 11.96), slightly metal-poor ([Fe/H] = - 0.55), G-type main-sequence star (T eff = 5891 K; $\\mathrm{log}g=4.07;$ R = 1.356R ⊙). This orbital period of 4.13 days would be the longest one for known redback candidates, which could hardly be understood for its formation in the standard recycling scenario due to its large Roche-lobe radius (≫the radius of the G-type main-sequence star). It is proposed here that this candidate redback millisecond pulsar binary could be created via accretion-induced collapse of an oxygen-neon-magnesium white dwarf.},
	keywords = {Neutron stars; 1108},
	year = {2024},
	eissn = {0004-637X},
	pages = {L5}
}

@article{MTMT:34514744,
	title = {New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World},
	url = {https://m2.mtmt.hu/api/publication/34514744},
	author = {Cadieux, Charles and Plotnykov, Mykhaylo and Doyon, René and Valencia, Diana and Jahandar, Farbod and Dang, Lisa and Turbet, Martin and Fauchez, Thomas J. and Cloutier, Ryan and Cherubim, Collin and Artigau, Étienne and Cook, Neil J. and Edwards, Billy and Hallatt, Tim and Charnay, Benjamin and Bouchy, François and Allart, Romain and Mignon, Lucile and Baron, Frédérique and Barros, Susana C. C. and Benneke, Björn and Canto, Martins B. L. and Cowan, Nicolas B. and De, Medeiros J. R. and Delfosse, Xavier and Delgado-Mena, Elisa and Dumusque, Xavier and Ehrenreich, David and Frensch, Yolanda G. C. and González, Hernández J. I. and Hara, Nathan C. and Lafrenière, David and Lo, Curto Gaspare and Malo, Lison and Melo, Claudio and Mounzer, Dany and Passeger, Vera Maria and Pepe, Francesco and Poulin-Girard, Anne-Sophie and Santos, Nuno C. and Sosnowska, Danuta and Suárez, Mascareño Alejandro and Thibault, Simon and Vaulato, Valentina and Wade, Gregg A. and Wildi, François},
	doi = {10.3847/2041-8213/ad1691},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {960},
	unique-id = {34514744},
	issn = {1538-4357},
	abstract = {The two-planet transiting system LHS 1140 has been extensively observed since its discovery in 2017, notably with Spitzer, HST, TESS, and ESPRESSO, placing strong constraints on the parameters of the M4.5 host star and its small temperate exoplanets, LHS 1140 b and c. Here, we reanalyze the ESPRESSO observations of LHS 1140 with the novel line-by-line framework designed to fully exploit the radial velocity content of a stellar spectrum while being resilient to outlier measurements. The improved radial velocities, combined with updated stellar parameters, consolidate our knowledge of the mass of LHS 1140 b (5.60 ± 0.19 M ⊕) and LHS 1140 c (1.91 ± 0.06 M ⊕) with an unprecedented precision of 3%. Transits from Spitzer, HST, and TESS are jointly analyzed for the first time, allowing us to refine the planetary radii of b (1.730 ± 0.025 R ⊕) and c (1.272 ± 0.026 R ⊕). Stellar abundance measurements of refractory elements (Fe, Mg, and Si) obtained with NIRPS are used to constrain the internal structure of LHS 1140 b. This planet is unlikely to be a rocky super-Earth, as previously reported, but rather a mini-Neptune with a ~0.1% H/He envelope by mass or a water world with a water-mass fraction between 9% and 19%, depending on the atmospheric composition and relative abundance of Fe and Mg. While the mini-Neptune case would not be habitable, a water-abundant LHS 1140 b potentially has habitable surface conditions according to 3D global climate models, suggesting liquid water at the substellar point for atmospheres with relatively low CO2 concentration, from Earth-like to a few bars.},
	keywords = {Habitable planets; EXOPLANETS; Astrophysics - Earth and Planetary Astrophysics; Super Earths; M dwarf stars; Planetary interior; 982; 498; 1655; 1248; 695},
	year = {2024},
	eissn = {0004-637X},
	pages = {L3}
}

@article{MTMT:34799248,
	title = {Assessing the Performance of the ADAPT and AFT Flux Transport Models Using In Situ Measurements from Multiple Satellites},
	url = {https://m2.mtmt.hu/api/publication/34799248},
	author = {Knizhnik, K.J. and Weberg, M.J. and Provornikova, E. and Warren, H.P. and Linton, M.G. and Shaik, S.B. and Ko, Y.-K. and Schonfeld, S.J. and Ugarte-Urra, I. and Upton, L.A.},
	doi = {10.3847/1538-4357/ad25f1},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {964},
	unique-id = {34799248},
	issn = {1538-4357},
	year = {2024},
	eissn = {0004-637X}
}

@article{MTMT:34796668,
	title = {Hydrodynamic Simulations of Oxygen–Neon Classical Novae as Galactic 7Li Producers and Potential Accretion-induced Collapse Progenitors},
	url = {https://m2.mtmt.hu/api/publication/34796668},
	author = {Starrfield, S. and Bose, M. and Iliadis, C. and Hix, W.R. and Woodward, C.E. and Wagner, R.M.},
	doi = {10.3847/1538-4357/ad1836},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {962},
	unique-id = {34796668},
	issn = {1538-4357},
	year = {2024},
	eissn = {0004-637X}
}

@article{MTMT:34786939,
	title = {Cosmology and Astrophysics with Standard Sirens and Galaxy Catalogs in View of Future Gravitational Wave Observations},
	url = {https://m2.mtmt.hu/api/publication/34786939},
	author = {Borghi, N. and Mancarella, M. and Moresco, M. and Tagliazucchi, M. and Iacovelli, F. and Cimatti, A. and Maggiore, M.},
	doi = {10.3847/1538-4357/ad20eb},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {964},
	unique-id = {34786939},
	issn = {1538-4357},
	year = {2024},
	eissn = {0004-637X}
}

@article{MTMT:34786673,
	title = {Host Galaxy and Nuclear Properties of IR-selected AGNs with and without Outflow Signatures},
	url = {https://m2.mtmt.hu/api/publication/34786673},
	author = {Oio, G.A. and Dai, Y.S. and Bornancini, C.G. and Li, Z.-J.},
	doi = {10.3847/1538-4357/ad18a5},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {962},
	unique-id = {34786673},
	issn = {1538-4357},
	year = {2024},
	eissn = {0004-637X}
}