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This work is based on data of NGC1316 from the Very Large Telescope
(VLT). We used B, V and I-band observations obtained with the FORS1
Imager at ESO’s VLT in Paranal (Program 64.H-0624(A), P.I. M. Della
The data reduction was carried out with the VST-Tube imaging pipeline.
VST-Tube is a very versatile software for astronomical data analysis,
tested against imaging data taken with different telescopes/detectors,
adaptable to existing or future multi-CCD cameras
(2 data files).
FIR-detected Lyman break galaxies at z ~ 3: Dust attenuation and dust correction factors at high redshift
Lyman break galaxies (LBGs) represent one of the kinds of star-forming
galaxies that are found in the high-redshift universe. The detection of
LBGs in the FIR domain can provide very important clues on their dust
attenuation and total SFR, allowing a more detailed study than those
performed so far. In this work we explore the FIR emission of a sample
of 16 LBGs at z ~ 3 in the GOODS-North and GOODS-South fields that are
individually detected in PACS-100um or PACS-160um. These detections
demonstrate the possibility of measuring the dust emission of LBGs at
high redshift. We find that…
The old nova V728 Sco has been recently recovered via photometric and
spectroscopic observations, 150 yr after the nova eruption. The spectral
properties pointed to a high-inclination system with a comparatively low
mass-transfer rate. In this paper, we show that the object is an
eclipsing system with an orbital period of 3.32 h. It has enhanced
long-term variability that can be interpreted as `stunted'
dwarf-nova-type outbursts. Using the ingress and egress times of the
eclipsed components we calculate the radius of the central object. The
latter turns out to be significantly larger than a…
T Pyx is a recurrent nova which has undergone eruptions on an almost
regular basis every 20 years until reaching a long lasting quiescence
between 1967 and 2011. We observed the long awaited 2011 explosion in
the optical and near infrared with intermediate spectral resolution. In
this paper we report on the change in the spectral type of the nova
(both during its rise and during its fading), as well as the observed
changes in the expansion velocities. We also present an interpretation
of these changes and set them in the general framework of a new
understanding of nova classification.