154 research outputs found
TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary
We report the discovery of a hot Jupiter on a 3.28-day orbit around a 1.08
M G0 star that is the secondary component in a loose binary system.
Based on follow-up radial velocity observations of TOI-858 B with CORALIE on
the Swiss 1.2 m telescope and CHIRON on the 1.5 m telescope at the Cerro Tololo
Inter-American Observatory (CTIO), we measured the planet mass to be M . Two transits were further observed with CORALIE to determine
the alignment of TOI-858 B b with respect to its host star. Analysis of the
Rossiter-McLaughlin signal from the planet shows that the sky-projected
obliquity is . Numerical simulations show that the
neighbour star TOI-858 A is too distant to have trapped the planet in a
Kozai-Lidov resonance, suggesting a different dynamical evolution or a
primordial origin to explain this misalignment. The 1.15 Msun primary F9 star
of the system (TYC 8501-01597-1, at ~11") was also observed with CORALIE
in order to provide upper limits for the presence of a planetary companion
orbiting that star.Comment: Accepted for publication in A&
MRC Centre Neuromuscular Biobank (Newcastle and London): Supporting and facilitating rare and neuromuscular disease research worldwide
Neuromuscular diseases are both genetic and acquired conditions resulting in progressive muscle weakness and wasting which lead to disability and reduced survival. The availability of high-quality human biomaterial is crucial to support biomedical research with potential applications at all stages of development, from molecular pathophysiology to drug discovery, clinical trials and evaluation of biomarkers. Although significant progress has been made over the last few years in the diagnosis of these rare conditions, the genetic defect and underlying pathological abnormality remain unknown in approximately 1/3 of cases. Moreover, to date no definitive cure is available for most neuromuscular disorders, nor are there sufficiently reliable and specific biomarkers to monitor disease progression and response to treatment. This is in part due to the rarity and genetic heterogeneity of neuromuscular diseases and the lack of access to patient samples. The availability of the national MRC Centre Biobank for Neuromuscular Diseases in Newcastle and London has addressed this bottleneck and supported neuromuscular research. Nine years after the establishment of the MRC Centre Biobank, many high profile research publications have highlighted the positive impact of neuromuscular biobanking for translational research and proven this facility to be a unique repository source for diagnostics, basic science research, industry, drug development, and therapy
Application of foam column as green technology for concentration of saponins from sisal (Agave sisalana) and Juá (Ziziphus joazeiro)
The young mini-Neptune HD 207496b that is either a naked core or on the verge of becoming one
We report the discovery and characterisation of the transiting mini-Neptune
HD~207496~b (TOI-1099) as part of a large programme that aims to characterise
naked core planets. We obtained HARPS spectroscopic observations, one
ground-based transit, and high-resolution imaging which we combined with the
TESS photometry to confirm and characterise the TESS candidate and its host
star. The host star is an active early K dwarf with a mass of M, a radius of R, and a G magnitude
of 8. We found that the host star is young, Myr, allowing us to
gain insight into planetary evolution. We derived a planetary mass of ,\, a planetary radius of ,\ and
a planetary density of .
From internal structure modelling of the planet, we conclude that the planet
has either a water-rich envelope, a gas-rich envelope, or a mixture of both. We
have performed evaporation modelling of the planet. If we assume the planet has
a gas-rich envelope, we find that the planet has lost a significant fraction of
its envelope and its radius has shrunk. Furthermore, we estimate it will lose
all its remaining gaseous envelope in Gyr. Otherwise, the planet
could have already lost all its primordial gas and is now a bare ocean planet.
Further observations of its possible atmosphere and/or mass-loss rate would
allow us to distinguish between these two hypotheses. Such observations would
determine if the planet remains above the radius gap or if it will shrink and
be below the gap.Comment: 20 pages, 18 figures, 4 tables, A&A accepte
NGTS discovery of a highly inflated Saturn-mass planet and a highly irradiated hot Jupiter: NGTS-26 b and NGTS-27 b
We report the discovery of two new transiting giant exoplanets NGTS-26 b and NGTS-27 b by the Next Generation Transit Survey (NGTS). NGTS-26 b orbits around a G6-type main sequence star every 4.52 days. It has a mass of 0.29-0.06+0.07 MJup and a radius of 1.33-0.05+0.06 RJup making it a Saturn-mass planet with a highly inflated radius. NGTS-27 b orbits around a slightly evolved G3-type star every 3.37 days. It has a mass of 0.59-0.07+0.10 MJup and a radius of 1.40±0.04 RJup, making it a relatively standard hot Jupiter. The transits of these two planetary systems were re-observed and confirmed in photometry by the SAAO 1.0-m telescope, 1.2-m Euler Swiss telescope as well as the TESS spacecraft, and their masses were derived spectroscopically by the CORALIE, FEROS and HARPS spectrographs. Both giant exoplanets are highly irradiated by their host stars and present an anomalously inflated radius, especially NGTS-26 b which is one of the largest objects among peers of similar mass
NGTS-13b: A hot 4.8 Jupiter-mass planet transiting a subgiant star
We report the discovery of the massive hot Jupiter NGTS-13b by the Next
Generation Transit Survey (NGTS). The V = 12.7 host star is likely in the
subgiant evolutionary phase with log g = 4.04 0.05, T =
5819 73 K, M = 1.30 M, and R =
1.79 0.06 R. NGTS detected a transiting planet with a period of
P = 4.12 days around the star, which was later validated with the Transiting
Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using
radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame
image photometry combined with CORALIE radial velocities we determine NGTS-13b
to have a radius of R = 1.142 0.046 R, mass of M =
4.84 0.44 M and eccentricity e = 0.086 0.034. Some previous
studies suggest that 4 M may be a border between two separate
formation scenarios (e.g., core accretion and disk instability) and that
massive giant planets share similar formation mechanisms as lower-mass brown
dwarfs. NGTS-13b is just above 4 M making it an important addition to
the statistical sample needed to understand the differences between various
classes of substellar companions. The high metallicity, [Fe/H] = 0.25
0.17, of NGTS-13 does not support previous suggestions that massive giants are
found preferentially around lower metallicity host stars, but NGTS-13b does
support findings that more massive and evolved hosts may have a higher
occurrence of close-in massive planets than lower-mass unevolved stars
NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event
We report the discovery of NGTS-11 b (=TOI-1847 b), a transiting Saturn in a
35.46-day orbit around a mid K-type star (Teff=5050 K). We initially identified
the system from a single-transit event in a TESS full-frame image light-curve.
Following seventy-nine nights of photometric monitoring with an NGTS telescope,
we observed a second full transit of NGTS-11 b approximately one year after the
TESS single-transit event. The NGTS transit confirmed the parameters of the
transit signal and restricted the orbital period to a set of 13 discrete
periods. We combined our transit detections with precise radial velocity
measurements to determine the true orbital period and measure the mass of the
planet. We find NGTS-11 b has a radius of 0.817+0.028-0.032 , a mass of
0.344+0.092-0.073 , and an equilibrium temperature of just 435+34-32 K,
making it one of the coolest known transiting gas giants. NGTS-11 b is the
first exoplanet to be discovered after being initially identified as a TESS
single-transit event, and its discovery highlights the power of intense
photometric monitoring in recovering longer-period transiting exoplanets from
single-transit events
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars From The Full-Frame Images
We present the discovery and characterization of five hot and warm Jupiters—TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960)—based on data from NASA\u27s Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (RP = 1.01–1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 \u3c V \u3c 10.8, 8.2 \u3c K \u3c 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars ( g \u3c 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (RP \u3e 1.7 RJ, possibly a result of its host star\u27s evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of MJ and a statistically significant, nonzero orbital eccentricity of e = . This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA\u27s TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals
Two long-period transiting exoplanets on eccentric orbits: NGTS-20 b (TOI-5152 b) and TOI-5153 b
Long-period transiting planets provide the opportunity to better understand
the formation and evolution of planetary systems. Their atmospheric properties
remain largely unaltered by tidal or radiative effects of the host star, and
their orbital arrangement reflects a different, and less extreme, migrational
history compared to close-in objects. The sample of long-period exoplanets with
well determined masses and radii is still limited, but a growing number of
long-period objects reveal themselves in the TESS data. Our goal is to vet and
confirm single transit planet candidates detected in the TESS space-based
photometric data through spectroscopic and photometric follow up observations
with ground-based instruments. We use the Next Generation Transit Survey (NGTS)
to photometrically monitor the candidates in order to observe additional
transits. We report the discovery of two massive, warm Jupiter-size planets,
one orbiting the F8-type star TOI-5153 and the other orbiting the G1-type star
NGTS-20 (=TOI-5152). From our spectroscopic analysis, both stars are metal-rich
with a metallicity of 0.12 and 0.15, respectively. Follow-up radial velocity
observations were carried out with CORALIE, CHIRON, FEROS, and HARPS. TOI-5153
hosts a 20.33 day period planet with a planetary mass of 3.26 (+-0.18) Mj, a
radius of 1.06 (+-0.04) Rj , and an orbital eccentricity of 0.091 (+-0.026).
NGTS-20 b is a 2.98 (+-0.16) Mj planet with a radius of 1.07 (+-0.04) Rj on an
eccentric (0.432 +- 0.023) orbit with an orbital period of 54.19 days. Both
planets are metal-enriched and their heavy element content is in line with the
previously reported mass-metallicity relation for gas giants. Both warm
Jupiters orbit moderately bright host stars making these objects valuable
targets for follow-up studies of the planetary atmosphere and measurement of
the spin-orbit angle of the system.Comment: 17 pages, 13 figures, accepted to A&
- …