المؤلفون: Tarantino, Umberto

مصطلحات موضوعية: Mathematics - Category Theory, Mathematics - Logic, 03G30, 18B25

الوصف: In this paper we further the study of arrow algebras, simple algebraic structures inducing toposes through the tripos-to-topos construction, by defining appropriate notions of morphisms between them which correspond to morphisms of the associated triposes. Specializing to geometric inclusions, we characterize subtriposes of an arrow tripos in terms of nuclei on the underlying arrow algebra, recovering a classical locale-theoretic result. As an example of application, we lift modified realizability to the setting of arrow algebras, and we establish its functoriality.

الوصول الحر: http://arxiv.org/abs/2407.02836Test

المؤلفون: Fisher, Deanne B., Bolatto, Alberto D., Chisholm, John, Fielding, Drummond, Levy, Rebecca C., Tarantino, Elizabeth, Boyer, Martha L., Cronin, Serena A., Lopez, Laura A., Smith, J. D., Berg, Danielle A., Lopez, Sebastian, Veilleux, Sylvain, van der Werf, Paul P., Böker, Torsten, Boogaard, Leindert A., Lenkić, Laura, Glover, Simon C. O., Villanueva, Vicente, Mayya, Divakara, Lai, Thomas S. -Y., Dale, Daniel A., Emig, Kimberly L., Walter, Fabian, Relaño, Monica, De Looze, Ilse, Mills, Elisabeth A. C., Leroy, Adam K., Meier, David S., Herrera-Camus, Rodrigo, Klessen, Ralf S.

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: In this paper we study the filamentary substructure of 3.3 $\mu$m PAH emission from JWST/NIRCam observations in the base of the M82 star-burst driven wind. We identify plume-like substructure within the PAH emission with widths of $\sim$50 pc. Several of the plumes extend to the edge of the field-of-view, and thus are at least 200-300 pc in length. In this region of the outflow, the vast majority ($\sim$70\%) of PAH emission is associated with the plumes. We show that those structures contain smaller scale "clouds" with widths that are $\sim$5-15 pc, and they are morphologically similar to the results of "cloud-crushing" simulations. We estimate the cloud-crushing time-scales of $\sim$0.5-3 Myr, depending on assumptions. We show this time scale is consistent with a picture in which these observed PAH clouds survived break-out from the disk rather than being destroyed by the hot wind. The PAH emission in both the midplane and the outflow is shown to tightly correlate with that of Pa$\alpha$ emission (from HST/NICMOS data), at the scale of both plumes and clouds, though the ratio of PAH-to-Pa$\alpha$ increases at further distances from the midplane. Finally, we show that the outflow PAH emission is suppressed in regions of the M82 wind that are bright in X-ray emission. Overall, our results are broadly consistent with a picture in which cold gas in galactic outflows is launched via hierarchically structured plumes, and those small scale clouds are more likely to survive the wind environment when collected into the larger plume structure.
Comment: Submitted to MNRAS

الوصول الحر: http://arxiv.org/abs/2405.03686Test

المؤلفون: Tarantino, Elizabeth, Bolatto, Alberto D., Indebetouw, Rémy, Rubio, Mónica, Sandstrom, Karin M., Smith, J. -D T., Stapleton, Daniel, Wolfire, Mark

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: We present Cloudy modeling of infrared emission lines in the Wolf-Rayet (WR) nebula N76 caused by one of the most luminous and hottest WR stars in the low metallicity Small Magellanic Cloud. We use spatially resolved mid-infrared Spitzer/IRS and far-infrared Herschel/PACS spectroscopy to establish the physical conditions of the ionized gas. The spatially resolved distribution of the emission allows us to constrain properties much more accurately than using spatially integrated quantities. We construct models with a range of constant hydrogen densities between n$_H$ = 4 - 10 cm$^{-3}$ and a stellar wind-blown cavity of 10 pc which reproduces the intensity and shape of most ionized gas emission lines, including the high ionization lines [OIV] and [NeV], as well as [SIII], [SIV], [OIII], and [NeIII]. Our models suggest that the majority of [SiII] emission (91%) is produced at the edge of the HII region around the transition between ionized and atomic gas while very little of the [CII] emission (<5%) is associated with the ionized gas. The physical conditions of N76 are characterized by a hot HII region with a maximum electron temperature of T$_e$ ~ 24,000 K, electron densities that range from n$_e$ ~ 4 to 12 cm$^{-3}$, and high ionization parameters of log(U) ~ -1.15 to -1.77. By analyzing a low metallicty WR nebula with a single ionization source, this work gives valuable insights on the impact WR stars have to the galaxy-integrated ionized gas properties in nearby dwarf galaxies.
Comment: 27 pages, 10 figures, 2 tables. Accepted in the Astrophysical Journal

الوصول الحر: http://arxiv.org/abs/2404.08041Test

المؤلفون: Green, Alex, Wong, Tony, Indebetouw, Remy, Nayak, Omnarayani, Bolatto, Alberto, Tarantino, Elizabeth, Rubio, Monica, Madden, Suzanne C., Hirschauer, Alec S.

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: To investigate the effects of stellar feedback on the gravitational state of giant molecular clouds (GMCs), we study $^{12}$CO and $^{13}$CO ALMA maps of nine GMCs distributed throughout the Large Magellanic Cloud (LMC), the nearest star-forming galaxy to our own. We perform noise and resolution matching on the sample, working at a common resolution of 3.5 arcseconds (0.85 pc at the LMC distance of 50 kpc), and use the \textit{SCIMES} clustering algorithm to identify discrete substructure, or "clumps." We supplement these data with three tracers of recent star formation: $8\mu$m surface brightness, continuum-subtracted H$\alpha$ flux, and interstellar radiation field energy density inferred from dust emission. The $^{12}$CO clumps identified cover a range of 3.6 dex in luminosity-based mass and 2.4 dex in average $8\mu$m surface brightness, representative of the wide range of conditions of the interstellar medium in the LMC. Our observations suggest evidence for increased turbulence in these clouds. While the turbulent linewidths are correlated with clump surface density, in agreement with previous observations, we find even better correlation with the three star formation activity tracers considered, suggesting stellar energy injection plays a significant role in the dynamical state of the clumps. The excess linewidths we measure do not appear to result from opacity broadening. $^{12}$CO clumps are found to be typically less gravitationally bound than $^{13}$CO clumps, with some evidence of the kinetic-to-gravitational potential energy ratio increasing with star-formation tracers. Further multi-line analysis may better constrain the assumptions made in these calculations.
Comment: 23 pages, 12 figures, accepted for publication in the Astrophysical Journal

الوصول الحر: http://arxiv.org/abs/2403.09594Test

المؤلفون: Bolatto, Alberto D., Levy, Rebecca C., Tarantino, Elizabeth, Boyer, Martha L., Fisher, Deanne B., Leroy, Adam K., Cronin, Serena A., Klessen, Ralf S., Smith, J. D., Berg, Dannielle A., Boeker, Torsten, Boogaard, Leindert A., Ostriker, Eve C., Thompson, Todd A., Ott, Juergen, Lenkic, Laura, Lopez, Laura A., Dale, Daniel A., Veilleux, Sylvain, van der Werf, Paul P., Glover, Simon C. O., Sandstrom, Karin M., Skillman, Evan D., Chisholm, John, Villanueva, Vicente, Lai, Thomas S. -Y., Lopez, Sebastian, Mills, Elisabeth A. C., Emig, Kimberly L., Armus, Lee, Maya, Divakara, Meier, David S., De Looze, Ilse, Herrera-Camus, Rodrigo, Walter, Fabian, Relano, Monica, Koziol, Hannah B., Marvil, Joshua, Jimenez-Donaire, Maria J., Martini, Paul

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find prominent plumes of PAH emission extending outward from the central starburst region, together with a network of complex filamentary substructure and edge-brightened bubble-like features. The structure of the PAH emission closely resembles that of the ionized gas, as revealed in Paschen alpha and free-free radio emission. We discuss the origin of the structure, and suggest the PAHs are embedded in a combination of neutral, molecular, and photoionized gas.
Comment: Submitted to The Astrophysical Journal

الوصول الحر: http://arxiv.org/abs/2401.16648Test

المؤلفون: Murray, Claire E., Hasselquist, Sten, Peek, Joshua E. G., Lindberg, Christina Willecke, Almeida, Andres, Choi, Yumi, Craig, Jessica E. M., Denes, Helga, Dickey, John M., Di Teodoro, Enrico M., Federrath, Christoph, Gerrard, Isabella A., Gibson, Steven J., Leahy, Denis, Lee, Min-Young, Lynn, Callum, Ma, Yik Ki, Marchal, Antoine, McClure-Griffiths, N. M., Nidever, David, Nguyen, Hiep, Pingel, Nickolas M., Tarantino, Elizabeth, Uscanga, Lucero, van Loon, Jacco Th.

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: The structure and dynamics of the star-forming disk of the Small Magellanic Cloud (SMC) have long confounded us. The SMC is widely used as a prototype for galactic physics at low metallicity, and yet we fundamentally lack an understanding of the structure of its interstellar medium (ISM). In this work, we present a new model for the SMC by comparing the kinematics of young, massive stars with the structure of the ISM traced by high-resolution observations of neutral atomic hydrogen (HI) from the Galactic Australian Square Kilometer Array Pathfinder survey (GASKAP-HI). Specifically, we identify thousands of young, massive stars with precise radial velocity constraints from the Gaia and APOGEE surveys and match these stars to the ISM structures in which they likely formed. By comparing the average dust extinction towards these stars, we find evidence that the SMC is composed of two structures with distinct stellar and gaseous chemical compositions. We construct a simple model that successfully reproduces the observations and shows that the ISM of the SMC is arranged into two, superimposed, star-forming systems with similar gas mass separated by ~5 kpc along the line of sight.
Comment: ApJ accepted. 20 pages, 18 figures

الوصول الحر: http://arxiv.org/abs/2312.07750Test

المؤلفون: Sarbadhicary, Sumit K., Wagner, Jordan, Koch, Eric W., Chen, Ness Mayker, Leroy, Adam K., Lahén, Natalia, Rosolowsky, Erik, Neugent, Kathryn F., Kim, Chang-Goo, Chomiuk, Laura, Dalcanton, Julianne J., Lopez, Laura A., Pingel, Nickolas M., Indebetouw, Remy, Williams, Thomas G., Tarantino, Elizabeth, Meyer, Jennifer Donovan, Skillman, Evan D., Smercina, Adam, Kepley, Amanda A., Murphy, Eric J., Strader, Jay, Wong, Tony, Stanimirović, Snežana, Villanueva, Vicente, Walter, Fabian, Ott, Juergen, Darling, Jeremy, Roman-Duval, Julia, Murray, Claire E.

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: Star formation in galaxies is regulated by turbulence, outflows, gas heating and cloud dispersal -- processes which depend sensitively on the properties of the interstellar medium (ISM) into which supernovae (SNe) explode. Unfortunately, direct measurements of ISM environments around SNe remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach: mapping the ISM around the massive stars that are soon to explode. This provides a much larger census of explosion sites than possible with only SNe, and allows comparison with sensitive, high-resolution maps of the atomic and molecular gas from the Jansky VLA and ALMA. In the well-resolved Local Group spiral M33, we specifically observe the environments of red supergiants (RSGs, progenitors of Type II SNe), Wolf-Rayet stars (WRs, tracing stars $>$30 M$_{\odot}$, and possibly future stripped-envelope SNe), and supernova remnants (SNRs, locations where SNe have exploded). We find that massive stars evolve not only in dense, molecular-dominated gas (with younger stars in denser gas), but also a substantial fraction ($\sim$45\% of WRs; higher for RSGs) evolve in lower-density, atomic-gas-dominated, inter-cloud media. We show that these measurements are consistent with expectations from different stellar-age tracer maps, and can be useful for validating SN feedback models in numerical simulations of galaxies. Along with the discovery of a 20-pc diameter molecular gas cavity around a WR, these findings re-emphasize the importance of pre-SN/correlated-SN feedback evacuating the dense gas around massive stars before explosion, and the need for high-resolution (down to pc-scale) surveys of the multi-phase ISM in nearby galaxies.
Comment: 34 pages, 14 figures. Submitted to ApJ. Comments welcome! The density distributions will be made publicly available after journal acceptance of manuscript. Please feel free to contact us in the meantime if you would like to use them

الوصول الحر: http://arxiv.org/abs/2310.17694Test

المؤلفون: Levy, Rebecca C., Bolatto, Alberto D., Tarantino, Elizabeth, Leroy, Adam K., Armus, Lee, Emig, Kimberly L., Herrera-Camus, Rodrigo, Marrone, Daniel P., Mills, Elisabeth, Ricken, Oliver, Stutzki, Juergen, Veilleux, Sylvain, Walter, Fabian

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: M82 is an archetypal starburst galaxy in the local Universe. The central burst of star formation, thought to be triggered by M82's interaction with other members in the M81 group, is driving a multiphase galaxy-scale wind away from the plane of the disk that has been studied across the electromagnetic spectrum. Here, we present new velocity-resolved observations of the [CII] 158$\mu$m line in the central disk and the southern outflow of M82 using the upGREAT instrument onboard SOFIA. We also report the first detections of velocity-resolved ($\Delta V = 10$ km s$^{-1}$) [CII] emission in the outflow of M82 at projected distances of $\approx1-2$ kpc south of the galaxy center. We compare the [CII] line profiles to observations of CO and HI and find that likely the majority ($>55$%) of the [CII] emission in the outflow is associated with the neutral atomic medium. We find that the fraction of [CII] actually outflowing from M82 is small compared to the bulk gas outside the midplane (which may be in a halo or tidal streamers), which has important implications for observations of [CII] outflows at higher redshift. Finally, by comparing the observed ratio of the [CII] and CO intensities to models of photodissociation regions, we estimate that the far-ultraviolet (FUV) radiation field in the disk is $\sim10^{3.5}~G_0$, in agreement with previous estimates. In the outflow, however, the FUV radiation field is 2-3 orders of magnitudes lower, which may explain the high fraction of [CII] arising from the neutral medium in the wind.
Comment: 22 pages, 9 figures, Accepted for publication in ApJ

الوصول الحر: http://arxiv.org/abs/2309.15906Test

المؤلفون: Maria Giuseppina Petruzzelli, Lucia Marzulli, Giuseppe Colacicco, Fabio Tarantino, Flora Furente, Alessandra Gabellone, Lucia Margari, Emilia Matera

المصدر: European Journal of Investigation in Health, Psychology and Education, Vol 14, Iss 5, Pp 1248-1259 (2024)

مصطلحات موضوعية: mental health, adolescence, self-harm, suicide, Public aspects of medicine, RA1-1270, Psychology, BF1-990

الوصف: Recent studies have revealed increasingly worse and more complex mental health conditions in young people, which is reflected in a growing trend in emergency room (ER) visits for acute psychopathological symptoms (APSs). This phenomenon has become exacerbated in recent decades, with a peak in the post-pandemic period. To better characterize the phenomenon, we investigated the change in the rate and type of ER counseling requests provided at the Child Neuropsychiatry Unit of the University Hospital of Bari, Italy over the period between 2019 and 2023 for subjects younger than 18 years old. For this purpose, we retrospectively analyzed a total number of 1073 urgent consultation reports retrieved through the reporting computerized operating system of our hospital. The distribution of the counseling requests provided for APSs and, among these, the distribution of the numbers of APSs and of the male: female ratio were significantly different over the years, with an increasing linear trend identified for APSs (p = 3.095 × 10−7), the average number of APSs (p = 3.598 × 10−7), and female gender prevalence (p = 0.03908), as well as for the patients with a history of psychotropic drug assumption (p = 0.0006319). A significant change in the number of urgent counseling requests received for eating disorders (p = 0.0007408), depression (p = 7.92 × 10−8), somatization (p = 4.03 × 10−6), self-harm (SA) (p = 1.358 × 10−6), and non-suicidal self-injury (NSSI) (p = 8.965 × 10−6) was found, with a significant increasing trend for anxiety (p = 0.0444), depression (p = 8.06 × 10−6), somatization (p = 0.004616), SA (p = 3.998 × 10−8), and NSSI (p = 5.074 × 10−7). The findings of our study support the hypothesis of an alarming progressive worsening of the mental health of children and adolescents, with an overlapping effect of the pandemic exacerbating the process.

وصف الملف: electronic resource

العلاقة: https://www.mdpi.com/2254-9625/14/5/82Test; https://doaj.org/toc/2174-8144Test; https://doaj.org/toc/2254-9625Test

الوصول الحر: https://doaj.org/article/8a29697bdbf348c181b4e41c256115bbTest

المؤلفون: UTfit Collaboration, Bona, Marcella, Ciuchini, Marco, Derkach, Denis, Ferrari, Fabio, Franco, Enrico, Lubicz, Vittorio, Martinelli, Guido, Morgante, Davide, Pierini, Maurizio, Silvestrini, Luca, Simula, Silvano, Stocchi, Achille, Tarantino, Cecilia, Vagnoni, Vincenzo, Valli, Mauro, Vittorio, Ludovico

مصطلحات موضوعية: High Energy Physics - Phenomenology, High Energy Physics - Experiment, High Energy Physics - Lattice

الوصف: Flavour mixing and CP violation as measured in weak decays and mixing of neutral mesons are a fundamental tool to test the Standard Model (SM) and to search for new physics. New analyses performed at the LHC experiment open an unprecedented insight into the Cabibbo-Kobayashi-Maskawa (CKM) metrology and new evidence for rare decays. Important progress has also been achieved in theoretical calculations of several hadronic quantities with a remarkable reduction of the uncertainties. This improvement is essential since previous studies of the Unitarity Triangle did show that possible contributions from new physics, if any, must be tiny and could easily be hidden by theoretical and experimental errors. Thanks to the experimental and theoretical advances, the CKM picture provides very precise SM predictions through global analyses. We present here the results of the latest global SM analysis performed by the UTfit collaboration including all the most updated inputs from experiments, lattice QCD and phenomenological calculations.
Comment: 24 pages, 7 figures, 11 tables

الوصول الحر: http://arxiv.org/abs/2212.03894Test