We analyse the rest-frame ultraviolet (UV) to near-infrared (near-IR)
spectral energy distribution (SED) of Lyman-break galaxies (LBGs),
star-forming (SF) BzK (sBzK) and UV-selected galaxies at 1.5 ≲ z
≲ 2.5 in the COSMOS, GOODS-N and GOODS-S fields. Additionally, we
complement the multiwavelength coverage of the galaxies located in the GOODS fields with deep far-infrared (FIR) data taken from the GOODS-Herschel project. According to their best-fitting SED-derived
properties we find that, because of their selection criterion involving
UV measurements, LBGs tend to be UV-brighter and bluer…
After the luminosity minimum of 2007-2008 (V=18.6, Polcaro et al. 2011,
AJ, 141, 18) and a moderate luminosity maximum at beginning 2011
(V=17.8), the Luminous Blue Variable GR290/Romano’s Star in M33 has
reached a new deep minimum with V=18.7 and R=18.4 in December 2013 which
appears to be the deepest so far recorded in its known light history.
Significant luminosity oscillations have been observed during the
2011-2013 declining phase.
La stella LBV (luminous blue variable) GR290 in M33, tenuta sotto controllo dalla nostra associazione, ha raggiunto un nuovo minimo di luminosità: rispetto al massimo avuto a Gennaio 2011, ora la stella è circa una magnitudine più debole su tutte le bande ottiche.
We study the characteristics of a narrow band type Ia supernova survey
through simulations based on the upcoming Javalambre Physics of the
accelerating universe Astrophysical Survey (J-PAS). This unique survey
has the capabilities of obtaining distances, redshifts, and the SN type
from a single experiment thereby circumventing the challenges faced by
the resource-intensive spectroscopic follow-up observations. We analyse
the flux measurements signal-to-noise ratio and bias, the supernova
typing performance, the ability to recover light curve parameters given
by the SALT2 model, the…
We present time-series photometric and spectroscopic data for seven old
novae. They are used to derive the orbital period for the systems: V365
Car (5.35 h), AR Cir (5.14 h), V972 Oph (6.75 h), HS Pup (6.41 h), V373
Sct (3.69 h), V909 Sgr (3.43 h) and CN Vel (5.29 h). Their addition
increases the number of orbital periods for novae by ˜10 per cent.
The eclipsing nature of V909 Sgr is confirmed, and in three other cases
(V365 Car, Ar Cir and V373 Sct) we detect significant photometric
orbital variability with amplitudes ≥0.2 mag in R. The resulting
period distribution is briefly discussed….
