In this paper we explore
This content will become publicly available on November 27, 2024
We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gammaray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phaseconnected rotation ephemerides are achieved. A further dozen optical and/or Xray binary systems colocated with LAT sources also likely harbor gammaray MSPs. This catalog thus reports roughly 340 gammaray pulsars and candidates, 10% of all known pulsars, compared to ≤11 known before Fermi. Half of the gammaray pulsars are young. Of these, the half that are undetected in radio have a broader Galactic latitude distribution than the young radioloud pulsars. The others are MSPs, with six undetected in radio. Overall, ≥236 are bright enough above 50 MeV to fit the pulse profile, the energy spectrum, or both. For the common twopeaked profiles, the gammaray peak closest to the magnetic pole crossing generally has a softer spectrum. The spectral energy distributions tend to narrow as the spindown power
 Award ID(s):
 1816904
 NSFPAR ID:
 10519064
 Author(s) / Creator(s):
 ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
 Publisher / Repository:
 American Astronomical Society
 Date Published:
 Journal Name:
 The Astrophysical Journal
 Volume:
 958
 Issue:
 2
 ISSN:
 0004637X
 Page Range / eLocation ID:
 191
 Format(s):
 Medium: X
 Sponsoring Org:
 National Science Foundation
More Like this

A<sc>bstract</sc> pp →W ^{±}(ℓ ^{±}ν )γ to in the SMEFT expansion. Calculations to this order are necessary to properly capture SMEFT contributions that grow with energy, as the interference between energyenhanced SMEFT effects at$$ \mathcal{O}\left(1/{\Lambda}^4\right) $$ $O\left(1/{\Lambda}^{4}\right)$ and the Standard Model is suppressed. We find that there are several dimension eight operators that interfere with the Standard Model and lead to the same energy growth, ~$$ \mathcal{O}\left(1/{\Lambda}^2\right) $$ $O\left(1/{\Lambda}^{2}\right)$ , as dimension six squared. While energyenhanced SMEFT contributions are a main focus, our calculation includes the complete set of$$ \mathcal{O}\left({E}^4/{\Lambda}^4\right) $$ $O\left({E}^{4}/{\Lambda}^{4}\right)$ SMEFT effects consistent with U(3)^{5}flavor symmetry. Additionally, we include the decay of the$$ \mathcal{O}\left(1/{\Lambda}^4\right) $$ $O\left(1/{\Lambda}^{4}\right)$W ^{±}→ ℓ ^{±}ν , making the calculation actually . As such, we are able to study the impact of nonresonant SMEFT operators, such as$$ \overline{q}{q}^{\prime}\to {\ell}^{\pm}\nu \gamma $$ $\overline{q}{q}^{\prime}\to {\ell}^{\pm}\mathrm{\nu \gamma}$$$ \left({L}^{\dagger }{\overline{\sigma}}^{\mu }{\tau}^IL\right)\left({Q}^{\dagger }{\overline{\sigma}}^{\nu }{\tau}^IQ\right) $$ $\left({L}^{\u2020}{\overline{\sigma}}^{\mu}{\tau}^{I}L\right)\left({Q}^{\u2020}{\overline{\sigma}}^{\nu}{\tau}^{I}Q\right)$B _{μν}, which contribute to directly and not to$$ \overline{q}{q}^{\prime}\to {\ell}^{\pm}\nu \gamma $$ $\overline{q}{q}^{\prime}\to {\ell}^{\pm}\mathrm{\nu \gamma}$ . We show several distributions to illustrate the shape differences of the different contributions.$$ \overline{q}{q}^{\prime}\to {W}^{\pm}\gamma $$ $\overline{q}{q}^{\prime}\to {W}^{\pm}\gamma $ 
Abstract Charge density wave (CDW) ordering has been an important topic of study for a long time owing to its connection with other exotic phases such as superconductivity and magnetism. The
($$R{\textrm{Te}}_{3}$$ $R{\text{Te}}_{3}$R = rareearth elements) family of materials provides a fertile ground to study the dynamics of CDW in van der Waals layered materials, and the presence of magnetism in these materials allows to explore the interplay among CDW and long range magnetic ordering. Here, we have carried out a highresolution angleresolved photoemission spectroscopy (ARPES) study of a CDW material , which is antiferromagnetic below$${\textrm{Gd}}{\textrm{Te}}_{3}$$ $\text{Gd}{\text{Te}}_{3}$ , along with thermodynamic, electrical transport, magnetic, and Raman measurements. Our ARPES data show a twofold symmetric Fermi surface with both gapped and ungapped regions indicative of the partial nesting. The gap is momentum dependent, maximum along$$\sim \mathrm {12~K}$$ $\sim 12\phantom{\rule{0ex}{0ex}}K$ and gradually decreases going towards$${\overline{\Gamma }}\mathrm{\overline{Z}}$$ $\overline{\Gamma}\overline{Z}$ . Our study provides a platform to study the dynamics of CDW and its interaction with other physical orders in two and threedimensions.$${\overline{\Gamma }}\mathrm{\overline{X}}$$ $\overline{\Gamma}\overline{X}$ 
Abstract Recently, the Hydrogen Epoch of Reionization Array (HERA) has produced the experiment’s first upper limits on the power spectrum of 21 cm fluctuations at
z ∼ 8 and 10. Here, we use several independent theoretical models to infer constraints on the intergalactic medium (IGM) and galaxies during the epoch of reionization from these limits. We find that the IGM must have been heated above the adiabaticcooling threshold byz ∼ 8, independent of uncertainties about IGM ionization and the radio background. Combining HERA limits with complementary observations constrains the spin temperature of thez ∼ 8 neutral IGM to 27 K 630 K (2.3 K $\u3008{\overline{T}}_{S}\u3009$ 640 K) at 68% (95%) confidence. They therefore also place a lower bound on Xray heating, a previously unconstrained aspects of early galaxies. For example, if the cosmic microwave background dominates the $\u3008{\overline{T}}_{S}\u3009$z ∼ 8 radio background, the new HERA limits imply that the first galaxies produced Xrays more efficiently than local ones. Thez ∼ 10 limits require even earlier heating if darkmatter interactions cool the hydrogen gas. If an extra radio background is produced by galaxies, we rule out (at 95% confidence) the combination of high radio and low Xray luminosities ofL _{r,ν}/SFR > 4 × 10^{24}W Hz^{−1} yr and ${M}_{\odot}^{1}$L _{X}/SFR < 7.6 × 10^{39}erg s^{−1} yr. The new HERA upper limits neither support nor disfavor a cosmological interpretation of the recent Experiment to Detect the Global EOR Signature (EDGES) measurement. The framework described here provides a foundation for the interpretation of future HERA results. ${M}_{\odot}^{1}$ 
Abstract The growth of supermassive black holes is strongly linked to their galaxies. It has been shown that the population mean black hole accretion rate (
) primarily correlates with the galaxy stellar mass ( $\overline{\mathrm{BHAR}}$M _{⋆}) and redshift for the general galaxy population. This work aims to provide the best measurements of as a function of $\overline{\mathrm{BHAR}}$M _{⋆}and redshift over ranges of 10^{9.5}<M _{⋆}< 10^{12}M _{⊙}andz < 4. We compile an unprecedentedly large sample with 8000 active galactic nuclei (AGNs) and 1.3 million normal galaxies from nine highquality survey fields following a wedding cake design. We further develop a semiparametric Bayesian method that can reasonably estimate and the corresponding uncertainties, even for sparsely populated regions in the parameter space. $\overline{\mathrm{BHAR}}$ is constrained by Xray surveys sampling the AGN accretion power and UVtoinfrared multiwavelength surveys sampling the galaxy population. Our results can independently predict the Xray luminosity function (XLF) from the galaxy stellar mass function (SMF), and the prediction is consistent with the observed XLF. We also try adding external constraints from the observed SMF and XLF. We further measure $\overline{\mathrm{BHAR}}$ for starforming and quiescent galaxies and show that starforming $\overline{\mathrm{BHAR}}$ is generally larger than or at least comparable to the quiescent $\overline{\mathrm{BHAR}}$ . $\overline{\mathrm{BHAR}}$ 
Abstract We derive a general expression for the absorptive part of the oneloop photon polarization tensor in a strongly magnetized quarkgluon plasma at nonzero baryon chemical potential. To demonstrate the application of the main result in the context of heavyion collisions, we study the effect of a nonzero baryon chemical potential on the photon emission rate. The rate and the ellipticity of photon emission are studied numerically as a function the transverse momentum (energy) for several values of temperature and chemical potential. When the chemical potential is small compared to the temperature, the rates of the quark and antiquark splitting processes (i.e.,
and$$q\rightarrow q +\gamma $$ $q\to q+\gamma $ , respectively) are approximately the same. However, the quark splitting gradually becomes the dominant process with increasing the chemical potential. We also find that increasing the chemical potential leads to a growing total photon production rate but has only a small effect on the ellipticity of photon emission. The quarkantiquark annihilation ($${\bar{q}}\rightarrow {\bar{q}} +\gamma $$ $\overline{q}\to \overline{q}+\gamma $ ) also contributes to the photon production, but its contribution remains relatively small for a wide range of temperatures and chemical potentials investigated.$$q+{\bar{q}}\rightarrow \gamma $$ $q+\overline{q}\to \gamma $