SPHERE dynamical and spectroscopic characterization of HD142527B.
R. Claudi, A.-L. Maire, D. Mesa, A. Cheetham, C. Fontanive, R. Gratton, A. Zurlo, H. Avenhaus, T. Bhowmik, B. Biller, A. Boccaletti, M. Bonavita, M. Bonnefoy, E. Cascone, G. Chauvin, A. Delboulbè, S. Desidera, V. D'Orazi, P. Feautrier, M. Feldt, F. Flammini Dotti, J.H. Girard, E. Giro, M. Janson, J. Hagelberg, M. Keppler, T. Kopytova, S. Lacour, A.-M. Lagrange, M. Langlois, J. Lannier, H. Le Coroller, F. Menard, S. Messina, M. Meyer, M. Millward, J. Olofsson, A. Pavlov, S. Peretti, C. Perrot, C. Pinte, J. Pragt, J. Ramos, S. Rochat, L. Rodet, R. Roelfsema, D. Rouan, G. Salter, T. Schmidt, E. Sissa, P. Thebault, S. Udry, A. Vigan
http://arxiv.org/abs/1812.07814
We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 MJ are visible in the field of view of IFS (\sim 100 au centered on the star) or in the IRDIS field of view (\sim 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M=0.11 \pm 0.06 MSun and R=0.15 \pm 0.07 RSun. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to accretion from infalling material. We consider that the spectral type of the secondary may also be earlier than the type we derived from IFS spectra. From dynamical considerations, we further constrain the mass to 0.26^{+0.16}_{-0.14} MSun , which is consistent with both our spectroscopic analysis and the values reported in the literature. Following previous methods, the lower and upper dynamical mass values correspond to a spectral type between M2.5 and M5.5 for the companion. By fitting the astrometric points, we find the following orbital parameters: a period of P=35-137 yr; an inclination of i=121-130 deg.; , a value of Omega=124-135 deg for the longitude of node, and an 68% confidence interval of \sim 18 - 57 au for the separation at periapsis. Eccentricity and time at periapsis passage exhibit two groups of values: \sim0.2-0.45 and \sim0.45-0.7 for e, and \sim 2015-2020 and \sim2020-2022 for T_0. While these orbital parameters might at first suggest that HD142527B is not the companion responsible for the outer disk truncation, a previous hydrodynamical analysis of this system showed that they are compatible with a companion that is able to produce the large cavity and other observed features.

Spectral and orbital characterisation of the directly imaged giant planet HIP 65426 b.
A. C. Cheetham, M. Samland, S. S. Brems, R. Launhardt, G. Chauvin, D. Segransan, T. Henning, A. Quirrenbach, H. Avenhaus, G. Cugno, J. Girard, N. Godoy, G. M. Kennedy, A.-L. Maire, S. Metchev, A. Mueller, A. Musso Barcucci, J. Olofsson, F. Pepe, S. P. Quanz, D. Queloz, S. Reffert, E. Rickman, R. van Boekel, A. Boccaletti, M. Bonnefoy, F. Cantalloube, B. Charnay, P. Delorme, M. Janson, M. Keppler, A.-M. Lagrange, M. Langlois, C. Lazzoni, F. Menard, D. Mesa, M. Meyer, T. Schmidt, E. Sissa, S. Udry, A. Zurlo
http://arxiv.org/abs/1812.07198
HIP 65426 b is a recently discovered Exoplanet imaged during the course of the SPHERE-SHINE survey. Here we present new L′L′ and M′M′ observations of the planet from the NACO instrument at the VLT from the NACO-ISPY survey, as well as a new Y−HY−H spectrum and KK-band photometry from SPHERE-SHINE. Using these data, we confirm the nature of the companion as a warm, dusty planet with a mid-L spectral type. From comparison of its SED with the BT-Settl atmospheric models, we derive a best-fit effective temperature of Teff=1618±7Teff=1618±7 K, surface gravity logg=3.78+0.04−0.03log⁡g=3.78−0.03+0.04 and radius R=1.17±0.04R=1.17±0.04 RJRJ (statistical uncertainties only). Using the DUSTY and COND isochrones we estimate a mass of 8±18±1 MJMJ. Combining the astrometric measurements from our new datasets and from the literature, we show the first indications of orbital motion of the companion (2.6σσ significance) and derive preliminary orbital constraints. We find a highly inclined orbit (i=107+13−10i=107−10+13 deg) with an orbital period of 800+1200−400800−400+1200 yr. We also report SPHERE sparse aperture maskingobservations that investigate the possibility that HIP 65426 b was scattered onto its current orbit by an additional companion at a smaller orbital separation. From this data we rule out the presence of Brown Dwarf companions with masses greater than 16 MJMJ at separations larger than 3 AU, significantly narrowing the parameter space for such a companion.

​​G. Cugno (1), S. P. Quanz (1), S. Hunziker (1), T. Stolker (1), H. M. Schmid (1), H. Avenhaus (2), P. Baudoz (3), A. J. Bohn (4), M. Bonnefoy (5), E. Buenzli (1), G. Chauvin (5 and 6), A. Cheetham (7), S. Desidera (8), C. Dominik (9), P. Feautrier (5), M. Feldt (2), C. Ginski (4), J. H. Girard (10), R. Gratton (8), J. Hagelberg (1), E. Hugot (11), M. Janson (12), A.-M. Lagrange (5), M. Langlois (11 and 13), Y. Magnard (5), A.-L. Maire (2), F. Menard (5 and 14), M. Meyer (15 and 1), J. Milli (10), C. Mordasini (16), C. Pinte (17 and 5), J. Pragt (18), R. Roelfsema (18), F. Rigal (18), J. Szulágyi (19), R. van Boekel (2), G. van der Plas (5), A. Vigan (11), Z. Wahhaj (10), A. Zurlo (11 and 20) ((1) ETH Zürich, (2) Max Planck Institute Heidelberg, (3) LESIA, (4) Leiden Observatory, (5) Univ. Grenoble, (6) Universidad de Chile, (7) Geneva Observatory, (8) Osservatorio Astronomico di Padova, (9) University of Amsterdam, (10) ESO Santiago de Chile, (11) Marseille Université, (12) Stockholm University, (13) CNRS Lyon, (14) CNRS Grenoble, (15) University of Michigan, (16) Universität Bern, (17) Monash University, (18) NOVA, (19) University of Zürich, (20) Universidad Diego Portales)
http://arxiv.org/abs/1812.06993
Aims: We want to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods: We analyzed observations of 6 young stars (age 3.5−103.5−10 Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the VLT in the Hαα filter (656 nm) and a nearby continuum filter (644.9 nm). Results: We re-detect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both Hαα and the continuum. We derive new astrometry (r=62.8+2.1−2.7r=62.8−2.7+2.1 mas and PA=(98.7±1.8)∘PA=(98.7±1.8)∘) and photometry (ΔΔN_Ha=6.3+0.2−0.36.3−0.3+0.2 mag, ΔΔB_Ha=6.7±0.26.7±0.2 mag and ΔΔCnt_Ha=7.3+0.3−0.27.3−0.2+0.3 mag) for the companion in agreement with previous studies, and estimate its mass accretion rate (M˙≈1−2×10−10M⊙ yr−1M˙≈1−2×10−10M⊙ yr−1). A faint point-like source around HD135344 B (SAO206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the locations of companion candidates around HD100546, HD169142 and MWC758 and calculate that processes involving Hαα fluxes larger than ∼8×10−14−10−15erg/s/cm2∼8×10−14−10−15erg/s/cm2 (M˙>10−10−10−12M⊙ yr−1M˙>10−10−10−12M⊙ yr−1) can be excluded. Furthermore, flux upper limits of ∼10−14−10−15erg/s/cm2∼10−14−10−15erg/s/cm2 (M˙<10−11−10−12M⊙ yr−1M˙<10−11−10−12M⊙ yr−1) are estimated within the gaps identified in the disks surrounding HD135344B and TW Hya.

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Dynamical masses of M-dwarf binaries in young moving groups: II - Toward empirical mass-luminosity isochrones.
Markus Janson, Stephen Durkan, Mickael Bonnefoy, Laetitia Rodet, Rainer Kohler, Sylvestre Lacour, Wolfgang Brandner, Thomas Henning, Julien Girard
http://arxiv.org/abs/1811.11802
Low-mass stars exhibit substantial pre-main sequence evolution during the first ~100 Myrs of their lives. Thus, young M-type stars are prime targets for isochronal dating, especially in young moving groups (YMGs), which contain large amounts of stars in this mass and age range. If the mass and luminosity of a star can both be directly determined, this allows for a particularly robust isochronal analysis. This motivates in-depth studies of low-mass binaries with spatially resolvable orbits, where dynamical masses can be derived. Here we present the results of an observing campaign dedicated to orbital monitoring of AB Dor Ba/Bb, which is a close M-dwarf pair within the quadruple AB Dor system. We have acquired eight astrometric epochs with the SPHERE/ZIMPOL and NACO instruments, which we combine with literature data to improve the robustness and precision for the orbital characterization of the pair. We find a system mass 0.66+/-0.12 Msun and bolometric luminosities in log(L/Lsun) of -2.02+/-0.02 and -2.11 +/- 0.02 for AB Dor Ba and Bb, respectively. These measurements are combined with other YMG pairs in the literature to start building a framework of empirical isochrones in mass-luminosity space. This can be used to calibrate theoretical isochrones and to provide a model-free basis for assessing relative stellar ages. We note a tentative emerging trend where the youngest moving group members are largely consistent with theoretical expectations, while stars in older associations such as the AB Dor moving group appear to be systematically underluminous relative to isochronal expectations.

So happy and proud for Jos (Jozua de Boer), my first PhD student who Yesterday defended a magnificent thesis (the blue book about "high contrast imaging of protoplanetary disks") in Leiden. We first met in 2012 and we "grew academically" together, me as ESO scientist and co-promotor (together with Prof.Dr Christoph Keller) and him as a student astronomer and now postdoc. I’m glad I could make it. PhD defenses in the Netherlands are really great. He gave a public talk in Dutch, and answered tough questions from a bunch of professors that looked as if they came out straight from the Hogwarts School of Witchcraft and Wizardry. It was a thrill to be sitting among them. Congratulations Dr de Boer and to the growing family!!!