Taurus Hill Observatory
Taurus Hill Observatory
Messina S.,National institute for astrophysics |
Millward M.,York Creek Observatory |
Buccino A.,CONICET |
Buccino A.,University of Buenos Aires |
And 22 more authors.
Astronomy and Astrophysics | Year: 2017
Aims. We intended to compile the most complete catalog of bona fide members and candidate members of the β Pictoris association, and to measure their rotation periods and basic properties from our own observations, public archives, and exploring the literature. Methods. We carried out a multi-observatories campaign to get our own photometric time series and collected all archived public photometric data time series for the stars in our catalog. Each time series was analyzed with the Lomb-Scargle and CLEAN periodograms to search for the stellar rotation periods. We complemented the measured rotational properties with detailed information on multiplicity, membership, and projected rotational velocity available in the literature and discussed star by star. Results. We measured the rotation periods of 112 out of 117 among bona fide members and candidate members of the β Pictoris association and, whenever possible, we also measured the luminosity, radius, and inclination of the stellar rotation axis. This represents to date the largest catalog of rotation periods of any young loose stellar association. Conclusions. We provided an extensive catalog of rotation periods together with other relevant basic properties useful to explore a number of open issues, such as the causes of spread of rotation periods among coeval stars, evolution of angular momentum, and lithium-rotation connection. © ESO, 2017.
Zheng W.,University of Michigan |
Shen R.F.,University of Toronto |
Sakamoto T.,NASA |
Sakamoto T.,University of Maryland Baltimore County |
And 60 more authors.
Astrophysical Journal | Year: 2012
We present a comprehensive analysis of a bright, long-duration (T 90 257 s) GRB 110205A at redshift z = 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb, and BOOTES telescopes when the gamma-ray burst (GRB) was still radiating in the γ-ray band, with optical light curve showing correlation with γ-ray data. Nearly 200 s of observations were obtained simultaneously from optical, X-ray, to γ-ray (1 eV to 5MeV), which makes it one of the exceptional cases to study the broadband spectral energy distribution during the prompt emission phase. In particular, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard synchrotron emission model in the fast cooling regime. Shortly after prompt emission (1100s), a bright (R = 14.0) optical emission hump with very steep rise (α 5.5) was observed, which we interpret as the reverse shock (RS) emission. It is the first time that the rising phase of an RS component has been closely observed. The full optical and X-ray afterglow light curves can be interpreted within the standard reverse shock (RS) + forward shock (FS) model. In general, the high-quality prompt and afterglow data allow us to apply the standard fireball model to extract valuable information, including the radiation mechanism (synchrotron), radius of prompt emission (R GRB 3 × 1013cm), initial Lorentz factor of the outflow (Γ0 250), the composition of the ejecta (mildly magnetized), the collimation angle, and the total energy budget. © 2012. The American Astronomical Society. All rights reserved..
Melandri A.,National institute for astrophysics |
Virgili F.J.,Liverpool John Moores University |
Bernardini M.G.,National institute for astrophysics |
Kobayashi S.,Liverpool John Moores University |
And 25 more authors.
Astronomy and Astrophysics | Year: 2014
The long Swift gamma-ray burst GRB? 120326A at redshift z = 1.798 exhibited a multi-band light-curve with a striking feature: a late-time, long-lasting achromatic rebrightening that is rarely seen in such events. Peaking in optical and X-ray bands ~35 ks (~12.5 ks in the GRB rest frame) after the 70 s GRB prompt burst, the feature brightened nearly two orders of magnitude above the underlying optical power-law decay. By modelling the multi-wavelength light-curves, we investigated possible causes of the rebrightening in the context of the standard fireball model. We excluded a range of scenarios for the origin of this feature: reverse-shock flash, late-time forward-shock peak caused by the passage of the brightest synchrotron frequency through the optical band, late central engine optical or X-ray flares, interaction between the expanding blast wave and a density enhancement in the circumburst medium, and gravitational microlensing. Instead we conclude that the achromatic rebrightening may be caused by a refreshed forward shock or a geometrical effect. In addition, we identify an additional component after the end of the prompt emission, which shapes the observed X-ray and optical light-curves differently, and which rules out a single overall emission component to explain the observed early-time emission. © ESO, 2014.
Baluev R.V.,Saint Petersburg State University |
Sokov E.N.,Russian Academy of Sciences |
Shaidulin V.S.,Saint Petersburg State University |
Sokova I.A.,Russian Academy of Sciences |
And 15 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2015
We perform an analysis of ~80 000 photometric measurements for the following 10 stars hosting transiting planets:WASP-2, -4, -5, -52, Kelt-1, CoRoT-2, XO-2, TrES-1, HD 189733, GJ 436. Our analysis includes mainly transit light curves from the Exoplanet Transit Database, public photometry from the literature, and some proprietary photometry privately supplied by other authors. Half of these light curves were obtained by amateurs. From this photometry we derive 306 transit timing measurements, as well as improved planetary transit parameters. Additionally, for 6 of these 10 stars we present a set of radial velocity measurements obtained from the spectra stored in the HARPS, HARPS-N and SOPHIE archives using the HARPS- TERRA pipeline. Our analysis of these transit timing and radial velocity data did not reveal significant hints of additional orbiting bodies in almost all of the cases. In the WASP-4 case, we found hints of marginally significant TTV signals having amplitude 10-20 s, although their parameters are model dependent and uncertain, while radial velocities did not reveal statistically significant Doppler signals. © 2015 The Authors.
Villforth C.,University of Turku |
Nilsson K.,University of Turku |
Heidt J.,ZAH |
Takalo L.O.,University of Turku |
And 45 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2010
OJ 287 is a BL Lac object at redshift.z= 0.306 that has shown double-peaked bursts at regular intervals of ∼12 yr during the last ∼40 yr. We analyse optical photopolarimetric monitoring data from 2005 to 2009, during which the latest double-peaked outburst occurred. The aim of this study is twofold: firstly, we aim to analyse variability patterns and statistical properties of the optical polarization light curve. We find a strong preferred position angle in optical polarization. The preferred position angle can be explained by separating the jet emission into two components: an optical polarization core and chaotic jet emission. The optical polarization core is stable on time-scales of years and can be explained as emission from an underlying quiescent jet component. The chaotic jet emission sometimes exhibits a circular movement in the Stokes plane. We find six such events, all on the time-scales of 10-20 d. We interpret these events as a shock front moving forwards and backwards in the jet, swiping through a helical magnetic field. Secondly, we use our data to assess different binary black hole models proposed to explain the regularly appearing double-peaked bursts in OJ 287. We compose a list of requirements a model has to fulfil to explain the mysterious behaviour observed in OJ 287. The list includes not only characteristics of the light curve but also other properties of OJ 287, such as the black hole mass and restrictions on accretion flow properties. We rate all existing models using this list and conclude that none of the models is able to explain all observations. We discuss possible new explanations and propose a new approach to understanding OJ 287. We suggest that both the double-peaked bursts and the evolution of the optical polarization position angle could be explained as a sign of resonant accretion of magnetic field lines, a 'magnetic breathing' of the disc. © 2010 The Authors. Journal compilation © 2010 RAS.
Takats K.,Andrés Bello University |
Takats K.,University of Szeged |
Pumo M.L.,National institute for astrophysics |
Elias-Rosa N.,National institute for astrophysics |
And 36 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2014
We present ultraviolet, optical, near-infrared photometry and spectroscopy of SN 2009N in NGC 4487. This object is a Type II-P supernova with spectra resembling those of subluminous II-P supernovae, while its bolometric luminosity is similar to that of the intermediate-luminosity SN 2008in. We created synow models of the plateau phase spectra for line identification and to measure the expansion velocity. In the near-infrared spectra we find signs indicating possible weak interaction between the supernova ejecta and the pre-existing circumstellar material. These signs are also present in the previously unpublished near-infrared spectra of SN 2008in. The distance to SN 2009N is determined via the expanding photosphere method and the standard candle method as D = 21.6 ± 1.1 Mpc. The produced nickel-mass is estimated to be ̃0.020 ± 0.004 M⊙. We infer the physical properties of the progenitor at the explosion through hydrodynamical modelling of the observables. We find the values of the total energy as ̃0.48 × 1051 erg, the ejected mass as ̃11.5 M⊙, and the initial radius as ̃287 R⊙. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Kankare E.,University of Turku |
Mattila S.,University of Turku |
Ryder S.,Australian Astronomical Observatory |
Fraser M.,University of Cambridge |
And 12 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2014
We present near-infrared and optical photometry, plus optical spectroscopy of two strippedenvelope supernovae (SNe) 2010O and 2010P that exploded in two different components of an interacting luminous infrared galaxy Arp 299 within only a few days of one another. SN 2010O is found to be photometrically and spectroscopically similar to many normal Type Ib SNe and our multiwavelength observations of SN 2010P suggest it to be a Type IIb SN. No signs of clear hydrogen features or interaction with the circumstellar medium are evident in the optical spectrum of SN 2010P. We derive estimates for the host galaxy line-of-sight extinctions for both SNe, based on both light curve and spectroscopic comparison finding consistent results. These methods are also found to provide much more robust estimates of the SN host galaxy reddening than the commonly used empirical relations between extinction and equivalent width of Na I D absorption features. The SN observations also suggest that different extinction laws are present in different components of Arp 299. For completeness, we study high-resolution pre-explosion images of Arp 299 and find both SNe to be close to, but not coincident with, extended sources that are likely massive clusters. A very simple model applied to the bolometric light curve of SN 2010O implies a rough estimate for the explosion parameters of Ek ≈ 3 × 1051 erg, Mej ≈ 2.9M⊙ and MNi ≈ 0.16M⊙. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Inserra C.,University of Catania |
Inserra C.,National institute for astrophysics |
Inserra C.,University of Oklahoma |
Turatto M.,National institute for astrophysics |
And 21 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2012
We present photometry and spectroscopy of the Type IIP supernova (SN IIP) 2009bw in UGC 2890 from a few days after the outburst to 241d. The light curve of SN 2009bw during the photospheric phase is similar to that of normal SNe IIP but with a brighter peak and plateau (mag, mag). The luminosity drop from the photospheric to the nebular phase is one of the fastest ever observed, ∼2.2mag in about 13d. The radioactive tail of the bolometric light curve indicates that the amount of ejected 56Ni is ≈0.022M ⊙. The photospheric spectra reveal high-velocity lines of Hα and Hβ until about 105d after the shock breakout, suggesting a possible early interaction between the SN ejecta and pre-existent circumstellar material, and the presence of CNO elements. By modelling the bolometric light curve, ejecta expansion velocity and photospheric temperature, we estimate a total ejected mass of ∼8-12M ⊙, a kinetic energy of ∼0.3 foe and an initial radius of ∼3.6-7 × 10 13cm. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.