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We present optical and near-infrared (NIR) observations of the Type Icn supernova (SN Icn) 2022ann, the fifth member of its newly identified class of SNe. Its early optical spectra are dominated by narrow carbon and oxygen P-Cygni features with absorption velocities of 800 km/s; slower than other SNe Icn and indicative of interaction with a dense, H/He-poor circumstellar medium (CSM) that is outflowing slower than a typical Wolf-Rayet wind velocity of $>$1000 km/s. We identify helium in NIR spectra obtained two weeks after maximum and in optical spectra at three weeks, demonstrating that the CSM is not fully devoid of helium. We never detect broad spectral features from SN ejecta, including in spectra extending to the nebular phase, a unique characteristic among SNe~Icn. Compared to other SNe Icn, SN 2022ann has a low luminosity, with a peak o-band absolute magnitude of -17.7, and evolves slowly. We model the bolometric light curve and find it is well-described by 1.7 M_Sun of SN ejecta interacting with 0.2 M_sun of CSM. We place an upper limit of 0.04 M_Sun of Ni56 synthesized in the explosion. The host galaxy is a dwarf galaxy with a stellar mass of 10^7.34 M_Sun (implied metallicity of log(Z/Z_Sun) $\approx$ 0.10) and integrated star-formation rate of log(SFR) = -2.20 M_sun/yr; both lower than 97\% of the galaxies observed to produce core-collapse supernovae, although consistent with star-forming galaxies on the galaxy Main Sequence. The low CSM velocity, nickel and ejecta masses, and likely low-metallicity environment disfavour a single Wolf-Rayet progenitor star. Instead, a binary companion star is likely required to adequately strip the progenitor before explosion and produce a low-velocity outflow. The low CSM velocity may be indicative of the outer Lagrangian points in the stellar binary progenitor, rather than from the escape velocity of a single Wolf-Rayet-like massive star., 21 pages, 13 figures, to be submitted to MNRAS

We present high-cadence photometric and spectroscopic observations of SN~2020jfo in ultraviolet and optical/near-infrared bands starting from $\sim 3$ to $\sim 434$ days after the explosion, including the earliest data with the 10.4\,m GTC. SN~2020jfo is a hydrogen-rich Type II SN with a relatively short plateau duration ($67.0 \pm 0.6$ days). When compared to other Type II supernovae (SNe) of similar or shorter plateau lengths, SN~2020jfo exhibits a fainter peak absolute $V$-band magnitude ($M_V = -16.90 \pm 0.34$ mag). SN~2020jfo shows significant H$\alpha$ absorption in the plateau phase similar to that of typical SNe~II. The emission line of stable [Ni~II] $\lambda$7378, mostly seen in low-luminosity SNe~II, is very prominent in the nebular-phase spectra of SN~2020jfo. Using the relative strengths of [Ni~II] $\lambda$7378 and [Fe~II] $\lambda$7155, we derive the Ni/Fe production (abundance) ratio of 0.08--0.10, which is $\sim 1.5$ times the solar value. The progenitor mass of SN~2020jfo from nebular-phase spectral modelling and semi-analytical modelling falls in the range of 12--15\,$M_\odot$. Furthermore, semi-analytical modelling suggests a massive H envelope in the progenitor of SN~2020jfo, which is unlikely for SNe~II having short plateaus.

We present high-cadence photometric and spectroscopic observations of SN~2020jfo in ultraviolet and optical/near-infrared bands starting from $\sim 3$ to $\sim 434$ days after the explosion, including the earliest data with the 10.4\,m GTC. SN~2020jfo is a hydrogen-rich Type II SN with a relatively short plateau duration ($67.0 \pm 0.6$ days). When compared to other Type II supernovae (SNe) of similar or shorter plateau lengths, SN~2020jfo exhibits a fainter peak absolute $V$-band magnitude ($M_V = -16.90 \pm 0.34$ mag). SN~2020jfo shows significant H$\alpha$ absorption in the plateau phase similar to that of typical SNe~II. The emission line of stable [Ni~II] $\lambda$7378, mostly seen in low-luminosity SNe~II, is very prominent in the nebular-phase spectra of SN~2020jfo. Using the relative strengths of [Ni~II] $\lambda$7378 and [Fe~II] $\lambda$7155, we derive the Ni/Fe production (abundance) ratio of 0.08--0.10, which is $\sim 1.5$ times the solar value. The progenitor mass of SN~2020jfo from nebular-phase spectral modelling and semi-analytical modelling falls in the range of 12--15\,$M_\odot$. Furthermore, semi-analytical modelling suggests a massive H envelope in the progenitor of SN~2020jfo, which is unlikely for SNe~II having short plateaus., Comment: 20 pages (plus 5 pages appendix), 19 figures, Accepted for publication in MNRAS

Supernovae are among the most powerful and influential explosions in the universe. They are also ideal multi-messenger laboratories to study extreme astrophysics. However, many fundamental properties of supernovae related to their diverse progenitor systems and explosion mechanisms remain poorly constrained. Here we outline how late-time spectroscopic observations obtained during the nebular phase (several months to years after explosion), made possible with the next generation of Extremely Large Telescopes, will facilitate transformational science opportunities and rapidly accelerate the community towards our goal of achieving a complete understanding of supernova explosions. We highlight specific examples of how complementary GMT and TMT instrumentation will enable high fidelity spectroscopy from which the line profiles and luminosities of elements tracing mass loss and ejecta can be used to extract kinematic and chemical information with unprecedented detail, for hundreds of objects. This will provide uniquely powerful constraints on the evolutionary phases stars may experience approaching a supernova explosion; the subsequent explosion dynamics; their nucleosynthesis yields; and the formation of compact objects that may act as central engines., Comment: 9 pages, 3 figures, Astro2020 Science White Paper

Interstellar and circumstellar matter.-- et al., The all-sky Planck survey in 9 frequency bands was used to search for emission from all 274 known Galactic supernova remnants. Of these, 16 were detected in at least two Planck frequencies. The radio-through-microwave spectral energy distributions were compiled to determine the mechanism for microwave emission. In only one case, IC 443, is there high-frequency emission clearly from dust associated with the supernova remnant. In all cases, the low-frequency emission is from synchrotron radiation. As predicted for a population of relativistic particles with energy distribution that extends continuously to high energies, a single power law is evident for many sources, including the Crab and PKS 1209-51/52. A decrease in flux density relative to the extrapolation of radio emission is evident in several sources. Their spectral energy distributions can be approximated as broken power laws, Sν ∝ ν−α, with the spectral index, α, increasing by 0.5–1 above a break frequency in the range 10–60 GHz. The break could be due to synchrotron losses., The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).

The involvement of the MET oncogene in de novo and acquired resistance of non-small cell lung cancers (NSCLCs) to tyrosine kinase inhibitors (TKIs) has previously been reported, but the precise mechanism by which MET overexpression contributes to TKI-resistant NSCLC remains unclear. MicroRNAs (miRNAs) negatively regulate gene expression, and their dysregulation has been implicated in tumorigenesis. To understand their role in TKI-resistant NSCLCs, we examined changes in miRNA that are mediated by tyrosine kinase receptors. Here we report that miR-30b, miR-30c, miR-221 and miR-222 are modulated by both epidermal growth factor (EGF) and MET receptors, whereas miR-103 and miR-203 are controlled only by MET. We showed that these miRNAs have important roles in gefitinib-induced apoptosis and epithelial-mesenchymal transition of NSCLC cells in vitro and in vivo by inhibiting the expression of the genes encoding BCL2-like 11 (BIM), apoptotic peptidase activating factor 1 (APAF-1), protein kinase C ɛ (PKC-ɛ) and sarcoma viral oncogene homolog (SRC). These findings suggest that modulation of specific miRNAs may provide a therapeutic approach for the treatment of NSCLCs.

Background: Apoptosis caused by endoplasmic reticulum (ER) stress contributes to atherothrombosis, the underlying cause of cardiovascular disease (CVD). T-cell death-associated gene 51 (TDAG51), a member of the pleckstrin homology-like domain gene family

In this paper we provide evidence on specific factors that could affect audit quality under mandatory rotation, using data from Korea where mandatory auditor rotation was put into effect in 2006. We find no evidence supporting the “Brillo pad effect” (the argument that departing auditors have incentives to clean up the balance sheet) or the “new broom effect” (the argument that new auditors can find problems that long-standing auditors tend to overlook). On the contrary, departing auditors spend fewer hours just before rotation, consistent with a lack of incentives to maintain quality given the impending rotation. Compared to clients in other mandatory rotations, the clients rotating away from industry specialist auditors have higher audit hours and higher absolute discretionary accruals post-rotation, suggesting there are adverse effects from breaking such auditor-client pairings. Finally we find that Big 4 auditors’ market share continues to increase after mandatory rotation is imposed. Our findings therefore fail to support mandatory rotation.

Although the hiring and firing of auditors by clients is believed to create a fundamental conflict of interest, there is little research on the issue except for experimental evidence in Mayhew and Pike (2004). To provide evidence on the issue, in this paper we exploit the setting in Korea, known as auditor designation, wherein regulators selectively and episodically selected auditors for certain client firms. We fail to find that audit quality proxied by absolute discretionary accruals, audit hours, modified opinions, and the tendency to meet or beat benchmarks, is higher for designated auditors. Our results therefore question whether hiring and firing of auditors by clients is a threat to auditor independence.

We present Spitzer MIPS SED and IRS observations of 14 Galactic Supernova Remnants previously identified in the GLIMPSE survey. We find evidence for SNR/molecular cloud interaction through detection of [OI] emission, ionic lines, and emission from molecular hydrogen. Through black-body fitting of the MIPS SEDs we find the large grains to be warm, 29-66 K. The dust emission is modeled using the DUSTEM code and a three component dust model composed of populations of big grains, very small grains, and polycyclic aromatic hydrocarbons. We find the dust to be moderately heated, typically by 30-100 times the interstellar radiation field. The source of the radiation is likely hydrogen recombination, where the excitation of hydrogen occurred in the shock front. The ratio of very small grains to big grains is found for most of the molecular interacting SNRs to be higher than that found in the plane of the Milky Way, typically by a factor of 2--3. We suggest that dust shattering is responsible for the relative over-abundance of small grains, in agreement with prediction from dust destruction models. However, two of the SNRs are best fit with a very low abundance of carbon grains to silicate grains and with a very high radiation field. A likely reason for the low abundance of small carbon grains is sputtering. We find evidence for silicate emission at 20 $\mu$m in their SEDs, indicating that they are young SNRs based on the strong radiation field necessary to reproduce the observed SEDs., Comment: Accepted in ApJ

International audience; We report on observations and theoretical interpretation of the explosion on comet 17P/Holmes 2007 Oct 23. Observed used the Spitzer mid-infrared spectrograph (5-40 microns), the Spitzer imaging photometer (24 and 70 microns), the Palomar Observatory 60-inch telescope, and frequent optical images from the Holloway comet observatory. The 2007 Nov 10 infrared spectral mapping revealed spatially diffuse emission with detailed mineralogical features, including those of small crystalline olivine grains. The 2008 Feb 27 spectra, and the central core of the 2007 Nov 10 spectral map, are nearly featureless, due to prevalence much larger grains that were ejected from the nucleus more slowly. The images and spectra in 2008 Mar can be segmented into three components: (1) a hemispherical shell due to the fastest (262 m/s), smallest (2 micron) debris; (2) a `blob' or `pseudonucleus' offset from the true nucleus, due to intermediate speed (93 m/s) and size (8 micron) particles; and (3) a `core' centered on the nucleus due to slower (9 m/s), larger (200 micron) ejecta. This decomposition of the mid-infrared observations also explains the temporal evolution of the mm-wave flux. The orientation of the leading edge of the ejecta shell and the ejecta `blob,' relative to the nucleus, do not change as the orientation of the Sun changes; instead, the configuration is imprinted by the orientation of the initial explosion. Using digitized versions of E. E. Barnard's images of the 1892 explosion of comet Holmes, we find remarkably similar properties of the explosion, including the direction of the ejecta remaining constant (rather than moving with the Sun). The earlier explosion was less energetic by a factor of about 20, meaning that the first and second most energetic cometary explosions witnessed by man are the 2007 and 1892 explosions of comet Holmes, in that order.

Cosmic Dust - Near and Far. 8-12 September 2008. Convention Center, Heidelberg, Germany., We present dust features and masses observed in young supernova remnants (SNRs) with Spitzer Infrared Spectrograph (IRS) mapping and staring observations of four youngest supernova remnants: SNR 1E102.2-7219 (E0102) in the Small Magellanic Cloud (SMC), Cas A and G11.2-0.3 in our Galaxy, and N132D in the Large Magellanic Cloud (LMC). The spectral mapping data revealed a number of dust features which include 21 micron-peak dust and featureless dust in Cas A and 18-micron peak dust in E0102 and N132D. The 18 micron-peak feature is fitted by a mix of MgSiO3 and solid Si dust grains, while the 21-micron peak dust is by a mix of silicates and FeO; we also explore dust fitting using Continuous Distribution of Ellipsoid grain models. We report detection of CO fundamental band from Cas A in near-infrared. We review dust features observed and identified in other SNRs. The dust emission is spatially correlated with the ejecta emission, showing dust is formed in SN ejecta. The spectra of E0102 show rich gas lines from ejecta including strong ejecta lines of Ne and O, including two [Ne III] lines and two [Ne V] lines which allow us to diagnostic density and temperature of the ejecta and measure the ejecta masses. E0102 and N132D show weak or lacking Ar, Si, and Fe ejecta, whereas the young Galactic SNR Cas A show strong Ar, Si, and S and weak Fe. We discuss compositions and masses of dust and association with those of ejecta and finally, dust contribution from SNe to early Universe.

We present Spitzer IRS and IRAC observations of the young supernova remnant E0102 (SNR 1E0102.2-7219) in the Small Magellanic Cloud. The infrared spectra show strong ejecta lines of Ne and O, with the [Ne II] line at 12.8 microns having a large velocity dispersion of 2,000-4,500 km/s indicative of fast-moving ejecta. Unlike the young Galactic SNR Cas A, E0102 lacks emission from Ar and Fe. Diagnostics of the observed [Ne III] line pairs imply that [Ne III] emitting ejecta have a low temperature of 650 K, while [Ne V] line pairs imply that the infrared [Ne V] emitting ejecta have a high density of ~10^4/cm3. We have calculated radiative shock models for various velocity ranges including the effects of photoionization. The shock model indicates that the [Ne V] lines come mainly from the cooling zone, which is hot and dense, whereas [Ne II] and [Ne III] come mainly from the photoinization zone, which has a low temperature of 400-1000 K. We estimate an infrared emitting Ne ejecta mass of 0.04 Msun from the infrared observations, and discuss implications for the progenitor mass. The spectra also have a dust continuum feature peaking at 18 microns that coincides spatially with the ejecta, providing evidence that dust formed in the expanding ejecta. The 18-micron-peak dust feature is fitted by a mixture of MgSiO3 and Si dust grains, while the rest of the continuum requires either carbon or Al2O3 grains. We measure the total dust mass formed within the ejecta of E0102 to be ~0.014 Msun. The dust mass in E0102 is thus a factor of a few smaller than that in Cas A. The composition of the dust is also different, showing relatively less silicate and likely no Fe-bearing dust, as is suggested by the absence of Fe-emitting ejecta., Comment: accepted by ApJ

We present Spitzer observations of IC 443 obtained with MIPS and IRS as part of our GTO program on the astrophysics of ejecta from evolved stars. We find that the overall morphology at mid/far IR wavelengths resembles even more closely a loop or a shell than the ground based optical and/or near IR images.The dust temperature map, based on the 70/160micron ratio, shows a range from 18 to 30 K degrees. The IRS spectra confirm the findings from previous near+mid IR spectroscopic observations of a collisionally excited gas, atomic and molecular, rich in fine structure atomic and pure H2 rotational emission lines, respectively. The spectroscopic shock indicator, [Ne II] 12.8micron, suggests shock velocities ranging from 60-90 km/s, consistent with the values derived from other indicators., Comment: 7 pages, 4 figures, PDF format only; to appear in the proceedings from "The Evolving ISM in the Milky Way and Nearby Galaxies"

An application framework for advanced image processing and visualization is presented. It provides common two-dimensional operators and implements recent developments in the field of image processing as well as original algorithms based on nonlinear partial differential equations (PDEs). It is platform independent and has the capability of extensibility. This objective is achieved by exploiting the object-oriented paradigm. A graphical user interface (GUI) provides processing, analysis and visualization in a highly integrated, easy to use environment. Applications of the developed system to images obtained by the Spitzer Space Telescope are demonstrated.

We present Spitzer IRAC images, with representative 5.27 to 38.5 micron IRSspectra, of the Cassiopeia A supernova remnant. Where each IRAC channel isdominant over the others, it illuminates different regions related to thenucleosynthetic layers of the progenitor star, echoing the inhomogeneitiesseen in the X-ray and optical. The Channel 1 (3.19 to 3.94microns) emission mechanism is synchrotron, but spectra towards Channel 1bright patches show a broad featureless continuum peaking around 26microns. We suggest that this is due to un-enriched circumstellar dustfrom the progenitor behind the outer shock and heated by the photons andelectrons from the shock as well as potentially processed (shattered,sputtered) by the shock. Where Channel 4 (6.45 to 9.38 microns) isdominant compared to the other IRAC channels, the spectra show astrong, 2-3 micron-wide peak at 21 microns, in addition to ionic lines of[ArII], [ArIII], [SIV] and [NeII], probably indicating where the shock haspenetrated into the oxygen- and silicon-burning layers. Thelong-wavelength continuum emission where Channel 3 (5.02 to 6.44microns) is dominant over the other channels rises gradually to 21microns, with a plateau to longer wavelengths. Channel 2 (4.02 to 5.03microns) depicts, in part, H recombination matching a Paschen beta emissionseen in the image obtained at Palomar, but spectra of strong Channel 2knots show a variety of broadband shapes. Where Channel 2 is very strongcompared to Channel 4, Channel 2 isolates regions where [ArII] is weakcompared to [NeII] in the spectra. In particular, Channels 2 and 3 areconsistent with line and dust emission reflecting only carbon- andneon-burning material. We suggest that all of these findings areconsistent with both the ionic and dust components delineating the distancethe reverse shockhas penetrated into the nucleosynthetic layers of the ejecta. Thepresence of Si and S in the remnant$apos;s interior, avoiding the Channel 4[ArII] regions, shows the distribution of the once-shocked (by the initialforward shock) material that has yet to be re-shocked by the reverse shockthat will heat it to X-ray temperatures. The patchy distribution ofdifferent elements at the reverse shock, in X-rays, optical, andinfrared, would then be due to hydrodynamic inhomogeneities deep in theprogenitor core, as opposed to major azimuthal variations in explosivenucleosynthesis.

Despite a general understanding that bone quality contributes to skeletal fragility, very little information exits on the age-dependent fatigue behavior of human bone. In this study four-point bending fatigue tests were conducted on aging bone in conjunction with the analysis of stiffness loss and preliminary investigation of nanoindentation based measurements of local tissue stiffness and histological evaluation of resultant tensile and compressive damage to identify the damage mechanism responsible for the increase in age-related bone fragility. The results obtained show that there is an exponential decrease in fatigue life with age, and old bone exhibits different modulus degradation profiles than young bone. In addition, this study provides preliminary evidence indicating that during fatigue loading, younger bone formed diffuse damage, lost local tissue stiffness on the tensile side. Older bone, in contrast, formed linear microcracks lost local tissue stiffness on the compressive side. Thus, the propensity of aging human bone to form more linear microcracks than diffuse damage may be a significant contributor to bone quality, and age related fragility in bone.

The optically-dark globule IC 1396A is revealed using Spitzer images at 3.6, 4.5, 5.8, 8, and 24 microns to be infrared-bright and to contain a set of previously unknown protostars. The mid-infrared colors of the 24 micon sources indicate several very young (Class I or 0) protostars and a dozen Class II stars. Three of the new sources emit over 90% of their bolometric luminosities at wavelengths greater than 3 microns, and they are located within ˜ 0.02 pc of the ionization front at the edge of the globule. Many of the sources have spectra that are still rising at 24 microns. The two previously-known young stars LkHalpha 349 a and c are both detected, with component c harboring a massive disk and component a being bare. Of order 5% of the mass of material in the globule is presently in the form of protostars in the 105--106 yr age range. This high star formation rate was likely triggered by radiation from a nearby O star.

Proper lymph node (LN) development requires tumor necrosis factor-related activation-induced cytokine (TRANCE) expression. Here we demonstrate that the defective LN development in TRANCE(-/)- mice correlates with a significant reduction in lymphotoxin (LT)alphabeta(+)alpha(4)beta(7)(+)CD45(+)CD4(+)CD3(-) cells and their failure to form clusters in rudimentary mesenteric LNs. Transgenic TRANCE overexpression in TRANCE(-/)- mice results in selective restoration of this cell population into clusters, and results in full LN development. Transgenic TRANCE-mediated restoration of LN development requires LTalphabeta expression on CD45(+) CD4(+)CD3(-) cells, as LNs could not be induced in LTalpha(-/)- mice. LTalpha(-/)- mice also showed defects in the fate of CD45(+)CD4(+)CD3(-) cells similar to TRANCE(-/)- mice. Thus, we propose that both TRANCE and LTalphabeta regulate the colonization and cluster formation by CD45(+) CD4(+)CD3(-) cells in developing LNs, the degree of which appears to correlate with the state of LN organogenesis.

Supernova remnants may exhibit both thermal and nonthermal X-ray emission. Such remnants can be distinguished by the weakness of their X-ray lines, because of the presence of a strong nonthermal X-ray continuum. RCW 86 is a remnant with weak lines, resulting in low and peculiar abundances when thermal models alone are used to interpret its X-ray spectrum. This indicates the presence of a strong nonthermal synchrotron continuum. We analyze ASCA X-ray spectra of RCW 86 with the help of both nonequilibrium ionization thermal models and nonthermal synchrotron models. A two-temperature thermal model and a simple nonthermal model with an exponential cutoff (plus interstellar absorption) give reasonable results. We obtain blast wave velocity of 800 km/s, the shock ionization age of 1-3x10^11 s/cm^3, and the break in nonthermal spectra at 2-4x10^16 Hz. The strength of nonthermal continuum correlates well with the radio brightness in the bright SW section of the remnant. This is convincing evidence for X-ray synchrotron emission in RCW 86., 14 pages, 11 figures, submitted to Astrophysical Journal