29 research outputs found
Shallow Ultraviolet Transits of WD 1145+017
WD 1145+017 is a unique white dwarf system that has a heavily polluted
atmosphere, an infrared excess from a dust disk, numerous broad absorption
lines from circumstellar gas, and changing transit features, likely from
fragments of an actively disintegrating asteroid. Here, we present results from
a large photometric and spectroscopic campaign with Hubble, Keck , VLT,
Spitzer, and many other smaller telescopes from 2015 to 2018. Somewhat
surprisingly, but consistent with previous observations in the u' band, the UV
transit depths are always shallower than those in the optical. We develop a
model that can quantitatively explain the observed "bluing" and the main
findings are: I. the transiting objects, circumstellar gas, and white dwarf are
all aligned along our line of sight; II. the transiting object is blocking a
larger fraction of the circumstellar gas than of the white dwarf itself.
Because most circumstellar lines are concentrated in the UV, the UV flux
appears to be less blocked compared to the optical during a transit, leading to
a shallower UV transit. This scenario is further supported by the strong
anti-correlation between optical transit depth and circumstellar line strength.
We have yet to detect any wavelength-dependent transits caused by the
transiting material around WD 1145+017.Comment: 16 pages, 11 figures, 6 tables, ApJ, in pres
Three Small Planets Transiting a Hyades Star
We present the discovery of three small planets transiting K2-136 (LP 358
348, EPIC 247589423), a late K dwarf in the Hyades. The planets have orbital
periods of , , and
days, and radii of , , and , respectively. With an age of
600-800 Myr, these planets are some of the smallest and youngest transiting
planets known. Due to the relatively bright (J=9.1) host star, the planets are
compelling targets for future characterization via radial velocity mass
measurements and transmission spectroscopy. As the first known star with
multiple transiting planets in a cluster, the system should be helpful for
testing theories of planet formation and migration.Comment: Accepted to The Astronomical Journa
The mass determination of TOI-519 b: a close-in giant planet transiting a metal-rich mid-M dwarf
We report the mass determination of TOI-519 b, a transiting substellar object
around a mid-M dwarf. We carried out radial velocity measurements using Subaru
/ InfraRed Doppler (IRD), revealing that TOI-519 b is a planet with a mass of
. We also find that the host star is metal
rich ( dex) and has the lowest effective
temperature ( K) among all stars hosting known
close-in giant planets based on the IRD spectra and mid-resolution infrared
spectra obtained with NASA Infrared Telescope Facility / SpeX. The core mass of
TOI-519 b inferred from a thermal evolution model ranges from to
, which can be explained by both the core accretion and disk
instability models as the formation origins of this planet. However, TOI-519 is
in line with the emerging trend that M dwarfs with close-in giant planets tend
to have high metallicity, which may indicate that they formed in the core
accretion model. The system is also consistent with the potential trend that
close-in giant planets around M dwarfs tend to be less massive than those
around FGK dwarfs.Comment: 10 pages, 5 figures. Accepted for publication in PAS
An M dwarf accompanied by a close-in giant orbiter with SPECULOOS
In the last decade, a dozen close-in giant planets have been discovered
orbiting stars with spectral types ranging from M0 to M4, a mystery since known
formation pathways do not predict the existence of such systems. Here, we
confirm TOI-4860 b, a Jupiter-sized planet orbiting an M4.5 host, a star at the
transition between fully and partially convective interiors. First identified
with TESS data, we validate the transiting companion's planetary nature through
multicolour photometry from the TRAPPIST-South/North, SPECULOOS, and MuSCAT3
facilities. Our analysis yields a radius of for
the planet, a mass of for the star, and an orbital period of
1.52 d. Using the newly commissioned SPIRIT InGaAs camera at the
SPECULOOS-South Observatory, we collect infrared photometry in zYJ that spans
the time of secondary eclipse. These observations do not detect a secondary
eclipse, placing an upper limit on the brightness of the companion. The
planetary nature of the companion is further confirmed through high-resolution
spectroscopy obtained with the IRD spectrograph at Subaru Telescope, from which
we measure a mass of . Based on its overall
density, TOI-4860 b appears to be rich in heavy elements, like its host star.Comment: Accepted for publication in MNRAS Letter
Two super-Earths at the edge of the habitable zone of the nearby M dwarf TOI-2095
The main scientific goal of TESS is to find planets smaller than Neptune
around stars bright enough to allow further characterization studies. Given our
current instrumentation and detection biases, M dwarfs are prime targets to
search for small planets that are in (or nearby) the habitable zone of their
host star. Here we use photometric observations and CARMENES radial velocity
measurements to validate a pair of transiting planet candidates found by TESS.
The data was fitted simultaneously using a Bayesian MCMC procedure taking into
account the stellar variability present in the photometric and spectroscopic
time series. We confirm the planetary origin of the two transiting candidates
orbiting around TOI-2095 (TIC 235678745). The star is a nearby M dwarf ( pc, K, mag) with a
stellar mass and radius of and , respectively. The planetary system is composed of
two transiting planets: TOI-2095b with an orbital period of days and TOI-2095c with days. Both planets have similar sizes with and for planet b and c,
respectively. We put upper limits on the masses of these objects with for the inner and for the outer planet
(95\% confidence level). These two planets present equilibrium temperatures in
the range of 300 - 350 K and are close to the inner edge of the habitable zone
of their star.Comment: Submitted to Astronomy & Astrophysic
First Detection of Two Superoutbursts during Rebrightening Phase of a WZ Sge-type Dwarf Nova: TCP J21040470+4631129
We report photometric and spectroscopic observations and analysis of the 2019
superoutburst of TCP J21040470+4631129. This object showed a 9-mag
superoutburst with early superhumps and ordinary superhumps, which are the
features of WZ Sge-type dwarf novae. Five rebrightenings were observed after
the main superoutburst. The spectra during the post-superoutburst stage showed
the Balmer, He I and possible sodium doublet features. The mass ratio is
derived as 0.0880(9) from the period of the superhump. During the third and
fifth rebrightenings, growing superhumps and superoutbursts were observed,
which have never been detected during a rebrightening phase among WZ Sge-type
dwarf novae with multiple rebrightenings. To induce a superoutburst during the
brightening phase, the accretion disk was needed to expand beyond the 3:1
resonance radius of the system again after the main superoutburst. These
peculiar phenomena can be explained by the enhanced viscosity and large radius
of the disk suggested by the higher luminosity and the presence of late-stage
superhumps during the post-superoutburst stage, plus by more mass supply from
the cool mass reservoir and/or from the secondary because of the enhanced mass
transfer than those of other WZ Sge-type dwarf novae.Comment: 13 pages, 10 figures, accepted for publication in PAS
First detection of two superoutbursts during rebrightening phase of a WZ Sge-type Dwarf Nova : TCP J21040470+4631129
We report on photometric and spectroscopic observations and analysis of the 2019 superoutburst of TCP J21040470+4631129. This object showed a 9 mag superoutburst with early superhumps and ordinary superhumps, which are the features of WZ Sge-type dwarf novae. Five rebrightenings were observed after the main superoutburst. The spectra during the post-superoutburst stage showed Balmer, He I, and possible sodium doublet features. The mass ratio is derived as 0.0880(9) from the period of the superhump. During the third and fifth rebrightenings, growing superhumps and superoutbursts were observed, which have never been detected during a rebrightening phase among WZ Sge-type dwarf novae with multiple rebrightenings. To induce a superoutburst during the brightening phase, the accretion disk needs to have expanded beyond the 3 : 1 resonance radius of the system again after the main superoutburst. These peculiar phenomena can be explained by the enhanced viscosity and large radius of the accretion disk suggested by the higher luminosity and the presence of late-stage superhumps during the post-superoutburst stage, plus by more mass supply from the cool mass reservoir and/or from the secondary because of the enhanced mass transfer than those of other WZ Sge-type dwarf novae.peer-reviewe
TOI-2046b, TOI-1181b, and TOI-1516b, three new hot Jupiters from TESS: planets orbiting a young star, a subgiant, and a normal star
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