Andrea S. J. Lin
A5057539235- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Astronomy and Astrophysical Research
- Astrophysics and Star Formation Studies
- Gamma-ray bursts and supernovae
- Astronomical Observations and Instrumentation
- Adaptive optics and wavefront sensing
- Atmospheric Ozone and Climate
- Space Exploration and Technology
- Solar and Space Plasma Dynamics
- Planetary Science and Exploration
- Spectroscopy and Laser Applications
- High-pressure geophysics and materials
- Geophysics and Gravity Measurements
- Advanced Fiber Optic Sensors
- Geomagnetism and Paleomagnetism Studies
- Scientific Computing and Data Management
- Scientific Measurement and Uncertainty Evaluation
- Mechanics and Biomechanics Studies
- Astrophysical Phenomena and Observations
- Calibration and Measurement Techniques
- Diverticular Disease and Complications
- COVID-19 and healthcare impacts
- Advanced Fiber Laser Technologies
Pennsylvania State University
2020-2024
Alexandra Hospital
2023
University of Alberta
2023
NASA Exoplanet Science Institute
2020
Abstract The warm Neptune GJ 3470b transits a nearby ( d = 29 pc) bright slowly rotating M1.5-dwarf star. Using spectroscopic observations during two with the newly commissioned NEID spectrometer on WIYN 3.5 m Telescope at Kitt Peak Observatory, we model classical Rossiter–McLaughlin effect, yielding sky-projected obliquity of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>λ</mml:mi> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>98</mml:mn>...
Abstract We present the discovery of TOI-5205b, a transiting Jovian planet orbiting solar metallicity M4V star, which was discovered using Transiting Exoplanet Survey Satellite photometry and then confirmed combination precise radial velocities, ground-based photometry, spectra, speckle imaging. TOI-5205b has one highest mass ratios for M-dwarf planets, with ratio almost 0.3%, as it orbits host star that is just 0.392 ± 0.015 M ⊙ . Its planetary radius 1.03 0.03 R J , while 1.08 0.06...
Abstract We confirm TOI-4201 b as a transiting Jovian-mass planet orbiting an early M dwarf discovered by the Transiting Exoplanet Survey Satellite. Using ground-based photometry and precise radial velocities from NEID Planet Finder Spectrograph, we measure mass of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>2.59</mml:mn> </mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.06</mml:mn> <mml:mo>+</mml:mo> <mml:mn>0.07</mml:mn>...
Abstract Recent discoveries of transiting giant exoplanets around M-dwarf stars (GEMS), aided by the all-sky coverage TESS, are starting to stretch theories planet formation through core-accretion scenario. upper limits on their occurrence suggest that they decrease with lower stellar masses, fewer GEMS lower-mass compared solar-type. In this paper, we discuss existing both confirmed planets, as well protoplanetary disk observations, and a combination tests reconcile these theoretical...
We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs. TOI-3714 ($V=15.24,~J=11.74$) is an M2 dwarf hosting a hot Jupiter ($M_p=0.70 \pm 0.03~\mathrm{M_J}$ and $R_p=1.01 0.03~\mathrm{R_J}$) on orbital period $2.154849 0.000001$ days with resolved white companion. TOI-3629 ($V=14.63,~J=11.42$) M1 ($M_p=0.26 0.02~\mathrm{M_J}$ $R_p=0.74 0.02~\mathrm{R_J}$) $3.936551_{-0.000006}^{+0.000005}$ days. characterize each transiting companion using combination...
Abstract We present the discovery of a low-density planet orbiting high-metallicity early M-dwarf TOI-5688 A b. This was characterized as part search for transiting giant planets ( R ≳ 8 ⊕ ) through Searching Giant Exoplanets around Stars (GEMS) survey. The discovered with Transiting Exoplanet Survey Satellite, and ground-based transits from Red Buttes Observatory, Table Mountain Observatory Pomona College, radial velocity (RV) measurements Habitable-Zone Planet Finder on 10 m Hobby Eberly...
Efforts with extreme-precision radial velocity (EPRV) instruments to detect small-amplitude planets are largely limited, on many timescales, by the effects of stellar variability and instrumental systematics. One avenue for investigating these is use small solar telescopes which direct disk-integrated sunlight EPRV instruments, observing Sun at high cadence over months or years. We have designed built a feed system carry out "Sun-as-a-star" observations NEID, very precision Doppler...
We present the discovery of a new Jovian-sized planet, TOI-3757 b, lowest density planet orbiting an M dwarf (M0V). It orbits solar-metallicity discovered using TESS photometry and confirmed with precise radial velocities (RV) from HPF NEID. With planetary radius $12.0^{+0.4}_{-0.5}$ $R_{\oplus}$ mass $85.3^{+8.8}_{-8.7}$ $M_{\oplus}$, not only does this object add to small sample gas giants ($\sim 10$) around dwarfs, but also, its low ($\rho =$ $0.27^{+0.05}_{-0.04}$ $\textrm{g~cm}^{-3}$)...
Abstract We perform an in-depth analysis of the recently validated TOI-3884 system, M4-dwarf star with a transiting super-Neptune. Using high-precision light curves obtained 3.5 m Apache Point Observatory and radial velocity observations Habitable-zone Planet Finder, we derive planetary mass <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>32.6</mml:mn> </mml:mrow> <mml:mo>−</mml:mo> <mml:mn>7.4</mml:mn> <mml:mo>+</mml:mo>...
We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs with stellar companions at wide separations. TOI-3984 A ($J=11.93$) is an M4 dwarf hosting a short-period ($4.353326 \pm 0.000005$ days) giant ($M_p=0.14\pm0.03~\mathrm{M_{J}}$ and $R_p=0.71\pm0.02~\mathrm{R_{J}}$) separation white companion. TOI-5293 ($J=12.47$) M3 ($2.930289 0.000004$ ($M_p=0.54\pm0.07~\mathrm{M_{J}}$ $R_p=1.06\pm0.04~\mathrm{R_{J}}$) characterize both systems using combination...
Abstract Giant exoplanets orbiting close to their host stars are unlikely have formed in present configurations 1 . These ‘hot Jupiter’ planets instead thought migrated inward from beyond the ice line and several viable migration channels been proposed, including eccentricity excitation through angular-momentum exchange with a third body followed by tidally driven orbital circularization 2,3 The discovery of extremely eccentric ( e = 0.93) giant exoplanet HD 80606 b (ref. 4 ) provided...
Abstract Transiting giant exoplanets around M-dwarf stars (GEMS) are rare, owing to the low-mass host stars. However, all-sky coverage of TESS has enabled detection an increasingly large number them enable statistical surveys like Searching for GEMS survey. As part this endeavor, we describe observations six transiting planets, which include precise mass measurements two (K2-419Ab, TOI-6034b) and validation four systems, includes upper limits three (TOI-5218b, TOI-5616b, TOI-5634Ab), while...
Abstract Stellar activity contamination of radial velocity (RV) data is one the top challenges plaguing field extreme-precision RV science. Previous work has shown that photometry can be very effective at removing such signals from data, especially stellar caused by rotating starspots and plage. The exact utility for contamination, best way to apply it, not well known. We present a combination photometric study eight Kepler/K2 FGK stars with known variability. use NEID RVs acquired...
Brown dwarfs bridge the gap between stars and planets, providing valuable insight into both planetary stellar formation mechanisms. Yet census of transiting brown dwarf companions, in particular around M stars, remains incomplete. We report discovery two low-mass hosts using a combination space- ground-based photometry along with near-infrared radial velocities. characterize TOI-5389Ab ($68.0^{+2.2}_{-2.2} \ \mj$) TOI-5610b ($40.4^{+1.0}_{-1.0} \mj$), moderately massive orbiting early...
Recent discoveries of transiting giant exoplanets around M dwarfs (GEMS) present an opportunity to investigate their atmospheric compositions and explore how such massive planets can form low-mass stars contrary canonical formation models. Here, we the first transmission spectra TOI-5205b, a short-period ($P=1.63~\mathrm{days}$) Jupiter-like planet ($M_p=1.08~\mathrm{M_J}$ $R_p=0.94~\mathrm{R_J}$) orbiting M4 dwarf. We obtained three transits using PRISM mode JWST Near Infrared Spectrograph...
Abstract We introduce NEIDSpecMatch , a tool developed to extract stellar parameters from spectra obtained with the NEID spectrograph. is based on SpecMatch-Emp and HPFSpecMatch which estimate by comparing observed spectrum well-characterized library spectra. This approach has proven effective for M dwarfs. Utilizing of 78 covering temperatures 3000–6000 K, derives key parameters, including temperature, metallicity, surface gravity, projected rotational velocity. Cross-validation shows...
NEID is a high-resolution red-optical precision radial velocity (RV) spectrograph recently commissioned at the WIYN 3.5 m telescope Kitt Peak National Observatory, Arizona, USA. has an extremely stable environmental control system, and spans wavelength range of 380 to 930 nm with two observing modes: High Resolution (HR) mode R $\sim$ 112,000 for maximum RV precision, Efficiency (HE) 72,000 faint targets. In this manuscript we present detailed description components NEID's optical fiber...
Abstract We obtained high-resolution spectra of the ultracool M-dwarf TRAPPIST-1 during transit its planet “b” using two high-dispersion near-infrared spectrographs, Infrared Doppler (IRD) instrument on Subaru 8.2m telescope, and Habitable Zone Planet Finder (HPF) 10 m Hobby–Eberly Telescope. These spectroscopic observations are complemented by a photometric observation for APO/ARCTIC, which assisted us in capturing correct times our spectroscopy. Using data new IRD HPF observations, as well...
Theories of planet formation predict that low-mass stars should rarely host exoplanets with masses exceeding Neptune. We used radial velocity observations to detect a Neptune-mass exoplanet orbiting LHS 3154, star is nine times less massive than the Sun. The exoplanet's orbital period 3.7 days, and its minimum mass 13.2 Earth masses. simulations show high planet-to-star ratio (>3.5 × 10-4) not an expected outcome either core accretion or gravitational instability theories formation. In...
Abstract We present an analysis of Sun-as-a-star observations from four different high-resolution, stabilized spectrographs—HARPS, HARPS-N, EXPRES, and NEID. With simultaneous the Sun instruments, we are able to gain insight into radial velocity precision accuracy delivered by each these instruments isolate instrumental systematics that differ true astrophysical signals. solar observations, can completely characterize expected Doppler shift contributed orbiting Solar System bodies remove...
Abstract TOI-2076 b is a sub-Neptune-sized planet ( R = 2.39 ± 0.10 ⊕ ) that transits young (204 50 MYr) bright V 9.2) K-dwarf hosting system of three transiting planets. Using spectroscopic observations obtained with the NEID spectrograph on WIYN 3.5 m Telescope, we model Rossiter–McLaughlin effect b, and derive sky-projected obliquity <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>λ</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow>...
We report the discovery of TOI-4127 b, a transiting, Jupiter-sized exoplanet on long-period ($P = 56.39879^{+0.00010}_{-0.00010}$ d), high-eccentricity orbit around late F-type dwarf star. This warm Jupiter was first detected and identified as promising candidate from search for single-transit signals in TESS Sector 20 data, later characterized planet following two subsequent transits (TESS Sectors 26 53) follow-up ground-based RV observations with NEID SOPHIE spectrographs. jointly fit...
Abstract TOI-1899 b is a rare exoplanet, temperate warm Jupiter orbiting an M dwarf, first discovered by Cañas et al. (2020) from TESS single-transit event. Using new radial velocities (RVs) the precision RV spectrographs HPF and NEID, along with additional photometry ground-based transit follow-up, we are able to derive much more precise orbital period of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>P</mml:mi> <mml:mo>=</mml:mo> <mml:msubsup>...
Abstract We confirm the planetary nature of TOI-1728b using a combination ground-based photometry, near-infrared Doppler velocimetry and spectroscopy with Habitable-zone Planet Finder. TOI-1728 is an old, inactive M0 star T eff = <?CDATA ${3980}_{-32}^{+31}$?> K, which hosts transiting super-Neptune at orbital period ∼3.49 days. Joint fitting radial velocities TESS transits yields radius ${5.05}_{-0.17}^{+0.16}$?> R ⊕ , mass ${26.78}_{-5.13}^{+5.43}$?> M eccentricity...
We confirm the planetary nature of TOI-532b, using a combination precise near-infrared radial velocities with Habitable-zone Planet Finder, TESS light curves, ground based photometric follow-up, and high-contrast imaging. TOI-532 is faint (J$\sim 11.5$) metal-rich M dwarf Teff = $3957\pm69$ K [Fe/H] $0.38\pm0.04$; it hosts transiting gaseous planet period $\sim 2.3$ days. Joint fitting ground-based transits reveal radius $5.82\pm0.19$ R$_{\oplus}$, mass $61.5_{-9.3}^{+9.7}$ M$_{\oplus}$....