146 research outputs found
A new and unusual LBV-like outburst from a Wolf–Rayet star in the outskirts of M33
MCA-1B (also called UIT003) is a luminous hot star in the western outskirts of M33, classified over 20 yr ago with a spectral type of Ofpe/WN9 and identified then as a candidate luminous blue variable (LBV). Palomar Transient Factory data reveal that this star brightened in 2010, with a light curve resembling that of the classic LBV star AF And in M31. Other Ofpe/WN9 stars have erupted as LBVs, but MCA-1B was unusual because it remained hot. It showed a WN-type spectrum throughout its eruption, whereas LBVs usually get much cooler. MCA-1B showed an almost four-fold increase in bolometric luminosity and a doubling of its radius, but its temperature stayed ≳29 kK. As it faded, it shifted to even hotter temperatures, exhibiting a WN7/WN8-type spectrum, and doubling its wind speed. MCA-1B is reminiscent of some supernova impostors, and its location resembles the isolated environment of SN 2009ip. It is most similar to HD 5980 (in the Small Magellanic Cloud) and GR 290 (also in M33). Whereas these two LBVs exhibited B-type spectra in eruption, MCA-1B is the first clear case where a Wolf–Rayet (WR) spectrum persisted at all times. Together, MCA-1B, HD 5980, and GR 290 constitute a class of WN-type LBVs, distinct from S Doradus LBVs. They are most interesting in the context of LBVs at low metallicity, a possible post-LBV/WR transition in binaries, and as likely Type Ibn supernova progenitors
SN2013fs and SN2013fr: Exploring the circumstellar-material diversity in Type II supernovae
We present photometry and spectroscopy of SN2013fs and SN2013fr in the first
100 days post-explosion. Both objects showed transient, relatively narrow
H emission lines characteristic of SNeIIn, but later resembled normal
SNeII-P or SNeII-L, indicative of fleeting interaction with circumstellar
material (CSM). SN2013fs was discovered within 8hr of explosion. Its light
curve exhibits a plateau, with spectra revealing strong CSM interaction at
early times. It is a less luminous version of the transitional SNIIn PTF11iqb,
further demonstrating a continuum of CSM interaction intensity between SNeII-P
and IIn. It requires dense CSM within 6.510~cm of the
progenitor, from a phase of advanced pre-SN mass loss shortly before explosion.
Spectropolarimetry of SN2013fs shows little continuum polarization, but
noticeable line polarization during the plateau phase. SN2013fr morphed from a
SNIIn at early times to a SNII-L. After the first epoch its narrow lines
probably arose from host-galaxy emission, but the bright, narrow H
emission at early times may be intrinsic. As for SN2013fs, this would point to
a short-lived phase of strong CSM interaction if proven to be intrinsic,
suggesting a continuum between SNeIIn and II-L. It is a low-velocity SNII-L,
like SN2009kr but more luminous. SN2013fr also developed an IR excess at later
times, due to warm CSM dust that require a more sustained phase of strong
pre-SN mass loss.Comment: MNRAS accepted. 28 pages, 23 figures, 8 table
SN2012ab: A Peculiar Type IIn Supernova with Aspherical Circumstellar Material
We present photometry, spectra, and spectropolarimetry of supernova (SN)
2012ab, mostly obtained over the course of days after discovery. SN
2012ab was a Type IIn (SN IIn) event discovered near the nucleus of spiral
galaxy 2MASXJ12224762+0536247. While its light curve resembles that of SN
1998S, its spectral evolution does not. We see indications of CSM interaction
in the strong intermediate-width emission features, the high luminosity (peak
at absolute magnitude ), and the lack of broad absorption features in
the spectrum. The H emission undergoes a peculiar transition. At early
times it shows a broad blue emission wing out to km
and a truncated red wing. Then at late times (
100days) it shows a truncated blue wing and a very broad red emission wing
out to roughly km . This late-time broad red wing
probably arises in the reverse shock. Spectra also show an asymmetric
intermediate-width H component with stronger emission on the red side
at late times. The evolution of the asymmetric profiles requires a density
structure in the distant CSM that is highly aspherical. Our spectropolarimetric
data also suggest asphericity with a strong continuum polarization of % and depolarization in the H line, indicating asphericity in the
CSM at a level comparable to that in other SNe IIn. We estimate a mass-loss
rate of for km extending back at least 75yr prior to the
SN. The strong departure from axisymmetry in the CSM of SN 2012ab may suggest
that the progenitor was an eccentric binary system undergoing eruptive mass
loss.Comment: 18 pages, 12 figure
A new and unusual LBV-like outburst from a Wolf–Rayet star in the outskirts of M33
MCA-1B (also called UIT003) is a luminous hot star in the western outskirts of M33, classified over 20 yr ago with a spectral type of Ofpe/WN9 and identified then as a candidate luminous blue variable (LBV). Palomar Transient Factory data reveal that this star brightened in 2010, with a light curve resembling that of the classic LBV star AF And in M31. Other Ofpe/WN9 stars have erupted as LBVs, but MCA-1B was unusual because it remained hot. It showed a WN-type spectrum throughout its eruption, whereas LBVs usually get much cooler. MCA-1B showed an almost four-fold increase in bolometric luminosity and a doubling of its radius, but its temperature stayed ≳29 kK. As it faded, it shifted to even hotter temperatures, exhibiting a WN7/WN8-type spectrum, and doubling its wind speed. MCA-1B is reminiscent of some supernova impostors, and its location resembles the isolated environment of SN 2009ip. It is most similar to HD 5980 (in the Small Magellanic Cloud) and GR 290 (also in M33). Whereas these two LBVs exhibited B-type spectra in eruption, MCA-1B is the first clear case where a Wolf–Rayet (WR) spectrum persisted at all times. Together, MCA-1B, HD 5980, and GR 290 constitute a class of WN-type LBVs, distinct from S Doradus LBVs. They are most interesting in the context of LBVs at low metallicity, a possible post-LBV/WR transition in binaries, and as likely Type Ibn supernova progenitors
Social defeat stress: Mechanisms underlying the increase in rewarding effects of drugs of abuse
Social interaction is known to be the main source of stress in human beings, which explains the translational importance of this research in animals. Evidence reported over the last decade has revealed that, when exposed to social defeat experiences (brief episodes of social confrontations during adolescence and adulthood), the rodent brain undergoes remodeling and functional modifications, which in turn lead to an increase in the rewarding and reinstating effects of different drugs of abuse. The mechanisms by which social stress cause changes in the brain and behavior are unknown, and so the objective of this review is to contemplate how social defeat stress induces long-lasting consequences that modify the reward system. First of all, we will describe the most characteristic results of the short- and long-term consequences of social defeat stress on the rewarding effects of drugs of abuse such as psychostimulants and alcohol. Secondly, and throughout the review, we will carefully assess the neurobiological mechanisms underlying these effects, including changes in the dopaminergic system, corticotrophin releasing factor signaling, epigenetic modifications and the neuroinflammatory response. To conclude, we will consider the advantages and disadvantages and the translational value of the social defeat stress model, and will discuss challenges and future directions
SN 2014ab: An Aspherical Type IIn Supernova with Low Polarization
We present photometry, spectra, and spectropolarimetry of supernova (SN)
2014ab, obtained through days after peak brightness. SN 2014ab was a
luminous Type IIn SN ( mag) discovered after peak brightness near
the nucleus of its host galaxy, VV 306c. Prediscovery upper limits constrain
the time of explosion to within 200 days prior to discovery. While SN 2014ab
declined by mag over the course of our observations, the observed
spectrum remained remarkably unchanged. Spectra exhibit an asymmetric
emission-line profile with a consistently stronger blueshifted component,
suggesting the presence of dust or a lack of symmetry between the far side and
near side of the SN. The Pa emission line shows a profile very similar
to that of H, implying that this stronger blueshifted component is
caused either through obscuration by large dust grains, occultation by
optically thick material, or a lack of symmetry between the far side and near
side of the interaction region. Despite these asymmetric line profiles, our
spectropolarimetric data show that SN 2014ab has little detected polarization
after accounting for the interstellar polarization. This suggests that we are
seeing emission from a photosphere that has only small deviation from circular
symmetry face-on. We are likely seeing a SN IIn with nearly circular symmetry
in the plane normal to our line of sight, but with either large-grain dust or
significant asymmetry in the density of circumstellar material or SN ejecta
along our line of sight. We suggest that SN 2014ab and SN 2010jl (as well as
other SNe IIn) may be similar events viewed from different directions.Comment: 20 pages, 19 figure
A new and unusual LBV-like outburst from a Wolf-Rayet star in the outskirts of M33
MCA-1B (also called UIT003) is a luminous hot star in the western outskirts
of M33, classified over 20yr ago with a spectral type of Ofpe/WN9 and
identified then as a candidate luminous blue variable (LBV). Palomar Transient
Factory data reveal that this star brightened in 2010, with a light curve
resembling that of the classic LBV star AFAnd in M31. Other Ofpe/WN9 stars have
erupted as LBVs, but MCA-1B was unusual because it remained hot. It showed a
WN-type spectrum throughout its eruption, whereas LBVs usually get much cooler.
MCA-1B showed an almost four-fold increase in bolometric luminosity and a
doubling of its radius, but its temperature stayed around 29kK. As it faded, it
shifted to even hotter temperatures, exhibiting a WN7/WN8-type spectrum, and
doubling its wind speed. MCA-1B is reminiscent of some supernova impostors, and
its location resembles the isolated environment of SN 2009ip. It is most
similar to HD5980 (in the SMC) and GR 290 (also in M33). Whereas these two LBVs
exhibited B-type spectra in eruption, MCA-1B is the first clear case where a
Wolf-Rayet (WR) spectrum persisted at all times. Together, MCA-1B, HD 5980, and
GR 290 constitute a class of WN-type LBVs, distinct from S Doradus LBVs. They
are most interesting in the context of LBVs at low metallicity, a possible
post-LBV/WR transition in binaries, and as likely Type~Ibn supernova
progenitors.Comment: accepted in MNRAS. 20 pages, 15 figure
The electron-capture origin of supernova 2018zd
In the transitional mass range ( 8-10 solar masses) between white dwarf
formation and iron core-collapse supernovae, stars are expected to produce an
electron-capture supernova. Theoretically, these progenitors are thought to be
super-asymptotic giant branch stars with a degenerate O+Ne+Mg core, and
electron capture onto Ne and Mg nuclei should initiate core collapse. However,
no supernovae have unequivocally been identified from an electron-capture
origin, partly because of uncertainty in theoretical predictions. Here we
present six indicators of electron-capture supernovae and show that supernova
2018zd is the only known supernova having strong evidence for or consistent
with all six: progenitor identification, circumstellar material, chemical
composition, explosion energy, light curve, and nucleosynthesis. For supernova
2018zd, we infer a super-asymptotic giant branch progenitor based on the faint
candidate in the pre-explosion images and the chemically-enriched circumstellar
material revealed by the early ultraviolet colours and flash spectroscopy. The
light-curve morphology and nebular emission lines can be explained with the low
explosion energy and neutron-rich nucleosynthesis produced in an
electron-capture supernova. This identification provides insights into the
complex stellar evolution, supernova physics, cosmic nucleosynthesis, and
remnant populations in the transitional mass range.Comment: Author version of the published letter in Nature Astronomy, 28 June
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Analytical bias in the measurement of serum 25-hydroxyvitamin D concentrations impairs assessment of vitamin D status in clinical and research settings
Measured serum 25-hydroxyvitamin D concentrations vary depending on the type of assay used and the specific laboratory undertaking the analysis, impairing the accurate assessment of vitamin D status. We investigated differences in serum 25-hydroxyvitamin D concentrations measured at three laboratories (laboratories A and B using an assay based on liquid chromatography-tandem mass spectrometry and laboratory C using a DiaSorin Liaison assay), against a laboratory using an assay based on liquid chromatography-tandem mass spectrometry that is certified to the standard reference method developed by the National Institute of Standards and Technology and Ghent University (referred to as the ‘ certified laboratory ’ ). Separate aliquots from the same original serum sample for a subset of 50 participants from the Ausimmune Study were analysed at the four laboratories. Bland-Altman plots were used to visually check agreement between each laboratory against the certified laboratory. Compared with the certified laboratory, serum 25-hydroxyvitamin D concentrations were on average 12.4 nmol/L higher at laboratory A (95% limits of agreement: -17 .8,42.6); 12.8 nmol/L higher at laboratory B (95% limits of agreement: 0.8,24.8); and 10.6 nmol/L lower at laboratory C (95% limits of agreement: -48.4,27.1). The prevalence of vitamin D deficiency (defined here as 25-hydroxyvitamin D < 50 nmol/L) was 24%, 16%, 12% and 41% at the certified laboratory, and laboratories A, B, and C, respectively. Our results demonstrate considerable differences in the measurement of 25-hydroxyvitamin D concentrations compared with a certified laboratory, even between laboratories using assays based on liquid chromatography-tandem mass spectrometry, which is often considered the gold-standard assay. To ensure accurate and reliable measurement of serum 25-hydroxyvitamin D concentrations, all laboratories should use an accuracy-based quality assurance system and, ideally, comply with international standardisation effort
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