R. Brahm

HATS-4b: A dense hot Jupiter transiting a super metal-rich G star

Development of the HATSouth project was funded by NSFMRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G and NNX12AH91H, and followup observations receive partial support from grant NSF/AST- 1108686. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and projects IC120009 “Millennium Institute of Astrophysics (MAS)” and P10-022-F of the Millennium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. acknowledges additional support from Nucleus P10-022-F of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. M.R. acknowledges support from FONDECYT postdoctoral fellowship 3120097. Australian access to the Magellan Telescopeswas supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the RobertMartin Ayers Sciences Fund, NASA’s Astrophysics Data System Bibliographic Services, and the SIMBADdatabase, operated at CDS, Strasbourg, France. Operations at the MPG/ESO 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory.

HATS-3b: An inflated hot Jupiter transiting an F-type star

We report the discovery by the HATSouth survey of HATS-3b, a transiting extrasolar planet orbiting a V=12.4 F dwarf star. HATS-3b has a period of P = 3.5479d, mass of Mp = 1.07MJ, and radius of Rp = 1.38RJ. Given the radius of the planet, the brightness of the host star, and the stellar rotational velocity (v sini = 9.0kms −1 ), this system will make an interesting target for future observations to measure the Rossiter-McLaughlin effect and determine its spin-orbit alignment. We detail the low/medium-resolution reconnaissance spectroscopy that we are now using to deal with large numbers of transiting planet candidates produced by the HATSouth survey. We show that this important step in discovering planets produces logg and Teff parameters at a precision suitable for efficient candidate vetting, as well as efficiently identifying stellar mass eclipsing binaries with radial velocity semi-amplitudes as low as 1kms −1 . Subject headings: planetary systems — stars: individual (HATS-3, GSC 6926-00454) techniques: spectroscopic, photometric

197 CANDIDATES AND 104 VALIDATED PLANETS IN K2's FIRST FIVE FIELDS

NASA through the Sagan Fellowship Program; NASA through a Hubble Fellowship - Space Telescope Science Institute; NASA [NAS 5-26555, NNH14CK55B]; National Science Foundation Graduate Research Fellowship [2014184874]; FONDECYT [1130857]; BASAL CATA [PFB-06]; Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio [IC 120009]; Alfred P. Sloan Foundation; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba Astronomical Foundation; Max Planck Institute for Astronomy; Heidelberg; Max Planck Institute for Extraterrestrial Physics, Garching; Johns Hopkins University; Durham University; University of Edinburgh; Queens University Belfast; Harvard-Smithsonian Center for Astrophysics; Las Cumbres Observatory Global Telescope Network Incorporated; National Central University of Taiwan; Space Telescope Science Institute; National Aeronautics and Space Administration [NNX08AR22G]; University of Maryland; Eotvos Lorand University (ELTE)

The mass-radius relationship for very low mass stars: Four new discoveries from the HATSouth Survey

Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX09AB29G and follow-up observations receive partial support from grant NSF/AST-1108686. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. Follow-up observations with the ESO 2.2 m/FEROS instrument were performed under MPI guaranteed time [P087.A9014(A), P088.A-9008(A), P089.A-9008(A)]. AJ acknowledges support from FONDECYT project 1130857, BASAL CATA PFB06 and the Millenium Science Initiative, Chilean Ministry of Economy (Nuclei: P10-022-F, P07-021-F). RB and NE are supported by CONICYT-PCHA/Doctorado Nacional and MR is supported by FONDECYT postdoctoral fellowship 3120097. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD data base, operated at CDS, Strasbourg, France. Operations at the MPG/ESO 2.2 m telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory.

HATS-6b: A warm saturn transiting an early m dwarf star, and a set of empirical relations for characterizing k and m dwarf planet hosts

We report the discovery by the HATSouth survey of HATS-6b, an extrasolar planet transiting a V=15.2 mag, i=13.7 mag M1V star with a mass of 0.57 Msun and a radius of 0.57 Rsun. HATS-6b has a period of P = 3.3253 d, mass of Mp=0.32 Mjup, radius of Rp=1.00 Rjup, and zero-albedo equilibrium temperature of Teq=712.8+-5.1 K. HATS-6 is one of the lowest mass stars known to host a close-in gas giant planet, and its transits are among the deepest of any known transiting planet system. We discuss the follow-up opportunities afforded by this system, noting that despite the faintness of the host star, it is expected to have the highest K-band S/N transmission spectrum among known gas giant planets with Teq < 750 K. In order to characterize the star we present a new set of empirical relations between the density, radius, mass, bolometric magnitude, and V, J, H and K-band bolometric corrections for main sequence stars with M < 0.80 Msun, or spectral types later than K5. These relations are calibrated using eclipsing binary components as well as members of resolved binary systems. We account for intrinsic scatter in the relations in a self-consistent manner. We show that from the transit-based stellar density alone it is possible to measure the mass and radius of a ~0.6 Msun star to ~7% and ~2% precision, respectively. Incorporating additional information, such as the V-K color, or an absolute magnitude, allows the precision to be improved by up to a factor of two.

HATS-2b: A transiting extrasolar planet orbiting a K-type star showing starspot activity

We report the discovery of HATS-2b, the second transiting extrasolar planet detected by the HATSouth survey. HATS-2b is moving on a circular orbit around a V = 13:6 mag, K-type dwarf star (GSC 6665-00236), at a separation of 0:0230 0:0003 AU and with a period of 1:3541 days. The planetary parameters have been robustly determined using a simultaneous fit of the HATSouth, MPG/ESO 2.2 m/GROND, Faulkes Telescope South/Spectral transit photometry, and MPG/ESO 2.2 m/FEROS, Euler 1.2 m/CORALIE, AAT 3.9 m/CYCLOPS radial-velocity measurements. HATS-2b has a mass of 1:37 0:16 MJ, a radius of 1:14 0:03 RJ, and an equilibrium temperature of 1567 30 K. The host star has a mass of 0:88 0:04 M and a radius of 0:89 0:02 R , and it shows starspot activity. We characterized the stellar activity by analyzing two photometric follow-up transit light curves taken with the GROND instrument, both obtained simultaneously in four optical bands (covering the wavelength range of 3860 9520 A). The two light curves contain anomalies compatible with starspots on the photosphere of the host star along the same transit chord.

Resolving the planetesimal belt of HR 8799 with ALMA

The star HR 8799 hosts one of the largest known debris discs and at least four giant planets. Previous observations have found evidence for a warm belt within the orbits of the planets, a cold planetesimal belt beyond their orbits and a halo of small grains. With the infrared data, it is hard to distinguish the planetesimal belt emission from that of the grains in the halo. With this in mind, the system has been observed with ALMA in band 6 (1.34 mm) using a compact array format. These observations allow the inner edge of the planetesimal belt to be resolved for the first time. A radial distribution of dust grains is fitted to the data using an MCMC method. The disc is best fitted by a broad ring between 145 +12 −12 au and 429

Search for associations containing young stars (SACY) - VII. New stellar and substellar candidate members in the young associations

Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M_⊙) owing to photometric survey sensitivities limiting the detections of lower mass objects. Aims. We search the field of view of 542 previously identified members of the young associations to identify wide or extremely wide (1000−100 000 au in physical separation) companions. Methods. We combined 2MASS near-infrared photometry (J, H, K) with proper motion values (from UCAC4, PPMXL, NOMAD) to identify companions in the field of view of known members. We collated further photometry and spectroscopy from the literature and conducted our own high-resolution spectroscopic observations for a subsample of candidate members. This complementary information allowed us to assess the efficiency of our method. Results. We identified 84 targets (45: 0.2−1.3 M_⊙, 17: 0.08−0.2 M_⊙, 22: <0.08 M_⊙) in our analysis, ten of which have been identified from spectroscopic analysis in previous young association works. For 33 of these 84, we were able to further assess their membership using a variety of properties (X-ray emission, UV excess, Hα, lithium and K I equivalent widths, radial velocities, and CaH indices). We derive a success rate of 76–88% for this technique based on the consistency of these properties. Conclusions. Once confirmed, the targets identified in this work would significantly improve our knowledge of the lower mass end of the young associations. Additionally, these targets would make an ideal new sample for the identification and study of planets around nearby young stars. Given the predicted substellar mass of the majority of these new candidate members and their proximity, high-contrast imaging techniques would facilitate the search for new low-mass planets.

New planetary systems from the Calan-Hertfordshire Extrasolar planet search

We report the discovery of eight new giant planets, and updated orbits for four known planets, orbiting dwarf and subgiant stars using the CORALIE, HARPS, and MIKE instruments as part of the Calan–Hertfordshire Extrasolar Planet Search. The planets have masses in the range 1.1–5.4 M J ’s, orbital periods from 40 to 2900 d, and eccentricities from 0.0 to 0.6. They include a double-planet system orbiting the most massive star in our sample (HD147873), two eccentric giant planets (HD128356 b and HD154672 b ), and a rare 14 Herculis analogue (HD224538 b ). We highlight some population correlations from the sample of radial velocity detected planets orbiting nearby stars, including the mass function exponential distribution, confirmation of the growing body of evidence that low-mass planets tend to be found orbiting more metal-poor stars than giant planets, and a possible period–metallicity correlation for planets with masses >0.1 M J , based on a metallicity difference of 0.16 dex between the population of planets with orbital periods less than 100 d and those with orbital periods greater than 100 d.

Early Optical Spectra of Nova V1369 Cen Show the Presence of Lithium

We present early high resolution spectroscopic observations of the nova V1369 Cen. We have detected an absorption feature at 6695.6 \AA\, that we have identified as blue--shifted