Magnetic, magnetocaloric and magnetotransport properties of RSn_{1+x}Ge_{1-x} compounds (R=Gd, Tb, Er; x=0.1)

We have studied the magnetic, magnetocaloric and magnetotransport properties of RSn1+xGe1-x(R=Gd, Tb, Er; x=0.1) series by means of magnetization, heat capacity and resistivity measurements. It has been found that all the compounds crystallize in the orthorhombic crystal structure described by the centrosymmetric space group Cmcm (No. 63). The magnetic susceptibility and heat capacity data suggest that all the compounds are antiferromagnetic. Large negative values of {\theta}p in case of GdSn1.1Ge0.9 and TbSn1.1Ge0.9 indicate that strong antiferromagnetic interactions are involved, which is also reflected in the magnetization isotherms. On the other hand ErSn1.1Ge0.9 shows weak antiferromagnetic interaction. The heat capacity data have been analyzed by fitting the temperature dependence and the values of {\theta}D and {\gamma} have been estimated. Among these three compounds, ErSn1.1Ge0.9 shows considerable magnetic entropy change of 9.5 J/kg K and an adiabatic temperature change of 3.2 K for a field of 50 kOe. The resistivity data in different temperature regimes have been analyzed and the dominant contributions have been identified. All the compounds show small but positive magnetoresistance.Comment: 23 pages,11 figure

Effect of Fe on the Martensitic Transition, Magnetic and Magnetocaloric Properties in Ni-Mn-In Melt-spun Ribbons

The effect of Fe on the martensitic transitions, magnetic and inverse magnetocaloric effect in Ni47Mn40-xFexIn13 ribbons (x = 1, 2, 3 and 5) has been investigated. All the ribbon compositions under study have shown the presence of austenite phase at room temperature. The variation of martensitic transition with the increase in Fe-content is non-monotonic. The thermal hysteresis of the martensitic transition increased with the increase in Fe-content. The martensitic transitions shifted to lower temperatures in the presence of high magnetic fields. A maximum magnetic entropy change (∆SM) of 50 Jkg-1K-1 has been achieved in the Ni47Mn38Fe2In13 (x = 1) ribbon at 282 K for an applied field of 5 T

Pressure-induced Changes In The Magnetic And Magnetocaloric Properties Of R Mn2 Ge2 (r=sm,gd)

We have studied the variation of magnetic and magnetocaloric properties of polycrystalline compounds SmMn2 Ge2 and GdMn2 Ge2 as a function of applied hydrostatic pressure. The magnetic transition temperatures are found to change considerably with pressure. The temperature regime of existence of antiferromagnetic (AFM) ordering is found to increase with pressure, in both the compounds. In SmMn2 Ge2, the sign of the magnetocaloric effect at the low-temperature ferromagnetic (FM)-AFM transition changes with pressure. The isothermal magnetic entropy change in this compound is found to increase by about 20 times as the pressure is increased from the ambient value to 6.8 kbar. Effect of pressure in GdMn2 Ge2 is less compared to that in SmMn2 Ge2. The variations in the magnetic and magnetocaloric properties are attributed to the changes in the magnetic state of the Mn sublattice under pressure. The difference in R-Mn coupling in Sm and Gd compounds is also found to play a role in determining the magnetic and magnetocaloric properties, both at ambient as well as under applied pressures. © 2008 The American Physical Society.7722Gschneidner Jr., K.A., Pecharsky, V.K., Tsokol, A.O., (2005) Rep. Prog. Phys., 68, p. 1479. , RPPHAG 0034-4885 10.1088/0034-4885/68/6/R04Tishin, A.M., Spichkin, Y.I., (2003) The Magnetocaloric Effect and Its Applications, , IOP, New YorkPecharsky, V.K., Gschneidner Jr., K.A., (1997) Phys. Rev. Lett., 78, p. 4494. , PRLTAO 0031-9007 10.1103/PhysRevLett.78.4494Gama, S., Coelho, A.A., De Campos, A., Carvalho, A.M.G., Gandra, F.C.G., Von Ranke, P.J., De Oliveira, N.A., (2004) Phys. Rev. Lett., 93, p. 237202. , PRLTAO 0031-9007 10.1103/PhysRevLett.93.237202Wada, H., Tanabe, Y., (2001) Appl. Phys. Lett., 79, p. 3302. , APPLAB 0003-6951 10.1063/1.1419048Fujii, H., Okamoto, T., Shigeoka, T., Iwata, N., (1985) Solid State Commun., 53, p. 715. , SSCOA4 0038-1098 10.1016/0038-1098(85)90385-0Fujii, H., Isoda, M., Okamoto, T., Shigeoka, T., Iwata, N., (1986) J. Magn. Magn. Mater., 54-57, p. 1345. , 0304-8853Sampathkumaran, E.V., Paulose, P.L., Mallik, R., (1996) Phys. Rev. B, 54, p. 3710. , PRBMDO 0163-1829 10.1103/PhysRevB.54.R3710Wada, H., Tanabe, Y., Hagiwara, K., Shiga, M., (2000) J. Magn. Magn. Mater., 218, p. 203. , JMMMDC 0304-8853 10.1016/S0304-8853(00)00410-8Fujiwara, T., Fujii, H., Shigeoka, T., (2001) Phys. Rev. B, 63, p. 174440. , PRBMDO 0163-1829 10.1103/PhysRevB.63.174440Barla, A., Sanchez, J.P., Malaman, B., Doyle, B.P., Rüffer, R., (2004) Phys. Rev. B, 69, p. 220405. , PRBMDO 0163-1829 10.1103/PhysRevB.69.220405Koyama, K., Miura, S., Okada, H., Shigeoka, T., Fujieda, S., Fujita, A., Fukamichi, K., Watanabe, K., (2006) J. Alloys Compd., 408-412, p. 118. , 0925-8388Han, Z., Wu, H., Wang, D., Hua, Z., Zhang, C., Gu, B., Du, Y., (2006) J. Appl. Phys., 100, p. 043908. , JAPIAU 0021-8979 10.1063/1.2266036Chaudhary, S., Chattopadhyay, M.K., Singh, K.J., Roy, S.B., Chaddah, P., Sampathkumaran, E.V., (2002) Phys. Rev. B, 66, p. 014424. , PRBMDO 0163-1829 10.1103/PhysRevB.66.014424Tomka, G.J., Ritter, C., Riedi, P.C., Kapusta, Cz., Kocemba, W., (1998) Phys. Rev. B, 58, p. 6330. , PRBMDO 0163-1829 10.1103/PhysRevB.58.6330Gerasimov, E.G., Mushnikov, N.V., Goto, T., (2005) Phys. Rev. B, 72, p. 064446. , PRBMDO 0163-1829 10.1103/PhysRevB.72.064446Koyama, K., Miura, S., Okada, H., Shigeoka, T., Watanabe, K., (2007) Mater. Trans., 48, p. 451. , MTARCE 1345-9678 10.2320/matertrans.48.451Kumar, P., Suresh, K.G., Nigam, A.K., Malik, S.K., (2007) J. Appl. Phys., 101, p. 013908. , JAPIAU 0021-8979 10.1063/1.2402975Kumar, P., Suresh, K.G., Nigam, A.K., Malik, S.K., (2008) J. Appl. Phys., 103, p. 013909. , JAPIAU 0021-8979 10.1063/1.2828179Fujiwara, T., Fujii, H., Shigeoka, T., (2001) Phys. Rev. B, 63, p. 174440. , PRBMDO 0163-1829 10.1103/PhysRevB.63.174440Welter, R., Venturini, G., Ressouche, E., Malman, B., (1995) J. Alloys Compd., 218, p. 204. , JALCEU 0925-8388 10.1016/0925-8388(94)01378-0Annaorazov, M.P., Nikitin, S.A., Tyurin, A.L., Asatryan, K.A., Kh. Dovletov, A., (1996) J. Appl. Phys., 79, p. 1689. , JAPIAU 0021-8979 10.1063/1.360955Yu, M.H., Levis, L.H., Moodenbaugh, A.R., (2003) J. Appl. Phys., 93, p. 10128. , JAPIAU 0021-8979 10.1063/1.1574591Wada, H., Yoshioka, H., Goto, T., (2002) J. Phys.: Condens. Matter, 14, p. 687. , JCOMEL 0953-8984 10.1088/0953-8984/14/41/10

Site-specific ubiquitination exposes a linear motif to promote interferon-α receptor endocytosis

Ligand-induced endocytosis and lysosomal degradation of cognate receptors regulate the extent of cell signaling. Along with linear endocytic motifs that recruit the adaptin protein complex 2 (AP2)–clathrin molecules, monoubiquitination of receptors has emerged as a major endocytic signal. By investigating ubiquitin-dependent lysosomal degradation of the interferon (IFN)-α/β receptor 1 (IFNAR1) subunit of the type I IFN receptor, we reveal that IFNAR1 is polyubiquitinated via both Lys48- and Lys63-linked chains. The SCFβTrcp (Skp1–Cullin1–F-box complex) E3 ubiquitin ligase that mediates IFNAR1 ubiquitination and degradation in cells can conjugate both types of chains in vitro. Although either polyubiquitin linkage suffices for postinternalization sorting, both types of chains are necessary but not sufficient for robust IFNAR1 turnover and internalization. These processes also depend on the proximity of ubiquitin-acceptor lysines to a linear endocytic motif and on its integrity. Furthermore, ubiquitination of IFNAR1 promotes its interaction with the AP2 adaptin complex that is required for the robust internalization of IFNAR1, implicating cooperation between site-specific ubiquitination and the linear endocytic motif in regulating this process

Erratum: "A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo" (2021, ApJ, 909, 218)

[no abstract available

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO-Virgo Run O3b

We search for gravitational-wave signals associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (2019 November 1 15:00 UTC-2020 March 27 17:00 UTC). We conduct two independent searches: A generic gravitational-wave transients search to analyze 86 GRBs and an analysis to target binary mergers with at least one neutron star as short GRB progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these GRBs. A weighted binomial test of the combined results finds no evidence for subthreshold gravitational-wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each GRB. Finally, we constrain the population of low-luminosity short GRBs using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate. © 2022. The Author(s). Published by the American Astronomical Society

Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run

Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours-months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets. © 2022. The Author(s). Published by the American Astronomical Society

GW190814: gravitational waves from the coalescence of a 23 solar mass black hole with a 2.6 solar mass compact object

We report the observation of a compact binary coalescence involving a 22.2–24.3 Me black hole and a compact object with a mass of 2.50–2.67 Me (all measurements quoted at the 90% credible level). The gravitational-wave signal, GW190814, was observed during LIGO’s and Virgo’s third observing run on 2019 August 14 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the three-detector network. The source was localized to 18.5 deg2 at a distance of - + 241 45 41 Mpc; no electromagnetic counterpart has been confirmed to date. The source has the most unequal mass ratio yet measured with gravitational waves, - + 0.112 0.009 0.008, and its secondary component is either the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system. The dimensionless spin of the primary black hole is tightly constrained to �0.07. Tests of general relativity reveal no measurable deviations from the theory, and its prediction of higher-multipole emission is confirmed at high confidence. We estimate a merger rate density of 1–23 Gpc−3 yr−1 for the new class of binary coalescence sources that GW190814 represents. Astrophysical models predict that binaries with mass ratios similar to this event can form through several channels, but are unlikely to have formed in globular clusters. However, the combination of mass ratio, component masses, and the inferred merger rate for this event challenges all current models of the formation and mass distribution of compact-object binaries

On the progenitor of binary neutron star merger GW170817

On 2017 August 17 the merger of two compact objects with masses consistent with two neutron stars was discovered through gravitational-wave (GW170817), gamma-ray (GRB 170817A), and optical (SSS17a/AT 2017gfo) observations. The optical source was associated with the early-type galaxy NGC 4993 at a distance of just ∼40 Mpc, consistent with the gravitational-wave measurement, and the merger was localized to be at a projected distance of ∼2 kpc away from the galaxy's center. We use this minimal set of facts and the mass posteriors of the two neutron stars to derive the first constraints on the progenitor of GW170817 at the time of the second supernova (SN). We generate simulated progenitor populations and follow the three-dimensional kinematic evolution from binary neutron star (BNS) birth to the merger time, accounting for pre-SN galactic motion, for considerably different input distributions of the progenitor mass, pre-SN semimajor axis, and SN-kick velocity. Though not considerably tight, we find these constraints to be comparable to those for Galactic BNS progenitors. The derived constraints are very strongly influenced by the requirement of keeping the binary bound after the second SN and having the merger occur relatively close to the center of the galaxy. These constraints are insensitive to the galaxy's star formation history, provided the stellar populations are older than 1 Gyr