X-ray emitting structures in the Vela SNR: ejecta anisotropies and progenitor stellar wind residuals. (arXiv:2103.09637v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sapienza_V/0/1/0/all/0/1">Vincenzo Sapienza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miceli_M/0/1/0/all/0/1">Marco Miceli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peres_G/0/1/0/all/0/1">Giovanni Peres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bocchino_F/0/1/0/all/0/1">Fabrizio Bocchino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orlando_S/0/1/0/all/0/1">Salvatore Orlando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greco_E/0/1/0/all/0/1">Emanuele Greco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combi_J/0/1/0/all/0/1">Jorge Ariel Combi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_F/0/1/0/all/0/1">Federico Garc&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sasaki_M/0/1/0/all/0/1">Manami Sasaki</a> The Vela supernova remnant (SNR) shows several ejecta fragments protruding beyond the forward shock (shrapnel). Recent studies have revealed high Si abundance in two shrapnel (A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G,Read More →

Caltech-NRAO Stripe 82 Survey (CNSS) Paper V: AGNs that transitioned to radio-loud state. (arXiv:2103.08422v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wolowska_A/0/1/0/all/0/1">Aleksandra Wo&#x142;owska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kunert_Bajraszewska_M/0/1/0/all/0/1">Magdalena Kunert-Bajraszewska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mooley_K/0/1/0/all/0/1">Kunal P. Mooley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siemiginowska_A/0/1/0/all/0/1">Aneta Siemiginowska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kharb_P/0/1/0/all/0/1">Preeti Kharb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishwara_Chandra_C/0/1/0/all/0/1">C. H. Ishwara-Chandra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallinan_G/0/1/0/all/0/1">Gregg Hallinan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gromadzki_M/0/1/0/all/0/1">Mariusz Gromadzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koziel_Wierzbowska_D/0/1/0/all/0/1">Dorota Kozie&#x142;-Wierzbowska</a> A recent multi-year Caltech-NRAO Stripe 82 Survey (CNSS) revealed a group of objects that appeared as new radio sources after $>$5–20 years of absence. They are transient phenomena with respect to the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) survey and constitute the first unbiased sample of renewed radio activity. Here we present the follow-up, radio, opticalRead More →

A Grid of Core-Collapse Supernova Remnant Models I: The Effect of Wind-Driven Mass-Loss. (arXiv:2103.07980v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Jacovich_T/0/1/0/all/0/1">Taylor Jacovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patnaude_D/0/1/0/all/0/1">Daniel Patnaude</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slane_P/0/1/0/all/0/1">Pat Slane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badenes_C/0/1/0/all/0/1">Carles Badenes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_S/0/1/0/all/0/1">Shiu-Hang Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagataki_S/0/1/0/all/0/1">Shigehiro Nagataki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milisavljevic_D/0/1/0/all/0/1">Dan Milisavljevic</a> Massive stars can shed material via steady, line-driven winds, eruptive outflows, or mass-transfer onto a binary companion. In the case of single stars, the mass is deposited by the stellar wind into the nearby environment. After the massive star explodes, the stellar ejecta interact with this circumstellar material (CSM), often-times resulting in bright X-ray line emission from both the shock-heated CSM and ejecta. The amount of material lostRead More →

A new, Gaia based, catalogue of blue straggler stars in open clusters. (arXiv:2103.06004v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Rain_M/0/1/0/all/0/1">M.J. Rain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahumada_J/0/1/0/all/0/1">J. Ahumada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carraro_G/0/1/0/all/0/1">G. Carraro</a> Blue straggler stars are exotic objects present in all stellar environments whose nature and formation channels are still partially unclear. They seem to be particularly abundant in open clusters (OCs), thus offering a unique chance to tackle these problems statistically.We aim to build up a new and homogeneous catalogue of blue straggler stars (BSS) in Galactic OCs using Gaia to provide a more solid assessment of the membership of these stars. We also aim to explore possible relationships of the stragglerRead More →

Deformed black hole in Sagittarius A. (arXiv:2103.05490v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Anson_T/0/1/0/all/0/1">Timothy Anson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Babichev_E/0/1/0/all/0/1">Eugeny Babichev</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Charmousis_C/0/1/0/all/0/1">Christos Charmousis</a> We analyze the Post-Newtonian orbit of stars around a deformed Kerr black hole. The deformation we consider is a class of disformal transformations of a non-trivial Kerr solution in scalar-tensor theory which are labeled via the disformal parameter $D$. We study different limits of the disformal parameter, and compare the trajectories of stars orbiting a black hole to the case of the Kerr spacetime in general relativity, up to 2PN order. Our findings show that for generic non-zero $D$, the no-hair theorem of general relativity is violated,Read More →

One-Dimensional Fuzzy Dark Matter Models: Structure Growth and Asymptotic Dynamics. (arXiv:2102.13619v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zimmermann_T/0/1/0/all/0/1">Tim Zimmermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwersenz_N/0/1/0/all/0/1">Nico Schwersenz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietroni_M/0/1/0/all/0/1">Massimo Pietroni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wimberger_S/0/1/0/all/0/1">Sandro Wimberger</a> This paper investigates the feasibility of simulating Fuzzy Dark Matter (FDM) with a reduced number of spatial dimensions. Our aim is to set up a realistic, yet numerically inexpensive, toy model in $(1+1)$-dimensional space time, that – under well controlled system conditions – is capable of realizing important aspects of the full-fledged $(3+1)$-FDM phenomenology by means of one-dimensional analogues. Based on the coupled, nonlinear and nonlocal $(3+1)$-Schr”odinger-Poisson equation under periodic boundary conditions, we derive two distinct one-dimensional models that differRead More →

Our Peculiar Motion Inferred from Number Counts of Mid Infra Red AGNs and the Discordance Seen with the Cosmological Principle. (arXiv:2102.12084v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Singal_A/0/1/0/all/0/1">Ashok K. Singal</a> The dipole anisotropy in the Cosmic Microwave Background Radiation (CMBR) has given a peculiar velocity vector 370 km s$^{-1}$ along $l=264^circ,b=48^circ$. However, some other dipoles, for instance, from the number counts, sky brightness or redshift distributions in large samples of distant Active Galactic Nuclei (AGNs), have yielded values of the peculiar velocity many times larger than that from the CMBR, though surprisingly, in all cases the directions agreed with the CMBR dipole. Here we determine our peculiar motionRead More →

Axi-Higgs Cosmology. (arXiv:2102.11257v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Fung_L/0/1/0/all/0/1">Leo WH Fung</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Li_L/0/1/0/all/0/1">Lingfeng Li</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Liu_T/0/1/0/all/0/1">Tao Liu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Luu_H/0/1/0/all/0/1">Hoang Nhan Luu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Qiu_Y/0/1/0/all/0/1">Yu-Cheng Qiu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tye_S/0/1/0/all/0/1">S.-H. Henry Tye</a> If the electroweak Higgs vacuum expectation value $v$ in early universe is $sim 1 %$ higher than its present value $v_0=246$ GeV, the $^7$Li puzzle in BBN and the CMB/$Lambda$CDM tension with late-universe measurements on Hubble parameter are mitigated. We propose a model of an axion coupled to the Higgs field, named “axi-Higgs”, with its mass $m_a sim 10^{-30} – 10^{-29},{rm eV}$ and decay constant $f_a sim 10^{17} – 10^{18},{rm GeV}$, to achieve this goal. The axion initial valueRead More →

Photometric Classifications of Evolved Massive Stars: Preparing for the Era of Webb and Roman with Machine Learning. (arXiv:2102.02829v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dorn_Wallenstein_T/0/1/0/all/0/1">Trevor Z. Dorn-Wallenstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davenport_J/0/1/0/all/0/1">James R.A. Davenport</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huppenkothen_D/0/1/0/all/0/1">Daniela Huppenkothen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levesque_E/0/1/0/all/0/1">Emily M. Levesque</a> In the coming years, next-generation space-based infrared observatories will significantly increase our samples of rare massive stars, representing a tremendous opportunity to leverage modern statistical tools and methods to test massive stellar evolution in entirely new environments. Such work is only possible if the observed objects can be reliably classified. Spectroscopic observations are infeasible with more distant targets, and so we wish to determine whether machine learning methods can classifyRead More →

Hierarchical Inference With Bayesian Neural Networks: An Application to Strong Gravitational Lensing. (arXiv:2010.13787v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_Carena_S/0/1/0/all/0/1">Sebastian Wagner-Carena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_J/0/1/0/all/0/1">Ji Won Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birrer_S/0/1/0/all/0/1">Simon Birrer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_P/0/1/0/all/0/1">Philip J. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roodman_A/0/1/0/all/0/1">Aaron Roodman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wechsler_R/0/1/0/all/0/1">Risa H. Wechsler</a> (for the LSST Dark Energy Science Collaboration) In the past few years, approximate Bayesian Neural Networks (BNNs) have demonstrated the ability to produce statistically consistent posteriors on a wide range of inference problems at unprecedented speed and scale. However, any disconnect between training sets and the distribution of real-world objects can introduce bias when BNNs are applied to data. This is a common challenge in astrophysics and cosmology, whereRead More →

A discovery of a low-energy excess in cosmic-ray iron: an evidence of the past supernova activity in the Local Bubble. (arXiv:2101.12735v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Boschini_M/0/1/0/all/0/1">M. J. Boschini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torre_S/0/1/0/all/0/1">S. Della Torre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gervasi_M/0/1/0/all/0/1">M. Gervasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grandi_D/0/1/0/all/0/1">D. Grandi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johannesson_G/0/1/0/all/0/1">G. Johannesson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vacca_G/0/1/0/all/0/1">G. La Vacca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masi_N/0/1/0/all/0/1">N. Masi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moskalenko_I/0/1/0/all/0/1">I. V. Moskalenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pensotti_S/0/1/0/all/0/1">S. Pensotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Porter_T/0/1/0/all/0/1">T. A. Porter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quadrani_L/0/1/0/all/0/1">L. Quadrani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rancoita_P/0/1/0/all/0/1">P. G. Rancoita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozza_D/0/1/0/all/0/1">D. Rozza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tacconi_M/0/1/0/all/0/1">M. Tacconi</a> Since its launch, the Alpha Magnetic Spectrometer – 02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species, $bar{p}$, $e^{pm}$, and nuclei, $_1$H-$_8$O, $_{10}$Ne, $_{12}$Mg, $_{14}$Si, which resulted in aRead More →

How will our knowledge on short gamma-ray burst affect the distance measurement of binary neutron star?. (arXiv:2101.12371v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Du_M/0/1/0/all/0/1">Minghui Du</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_L/0/1/0/all/0/1">Lixin Xu</a> Binary neutron star associated with short gamma-ray burst has drawn wide attention ever since the observation of GW170817, due to its prospect in cosmology. While further application of this sort of event suffers from the problem of degeneracy between luminosity distance and inclination angle. To address this issue, proposed in previous research is the utilization of information from short gamma-ray burst. In this paper, we aim to investigate the effect of different Gaussian priors of the inclination angle. To testRead More →

Detection of the atomic hydrogen (HI) absorption line and continuum emission from comet C/2020 F3 (NEOWISE) using GMRT. (arXiv:2101.05267v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pal_S/0/1/0/all/0/1">Sabyasachi Pal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manna_A/0/1/0/all/0/1">Arijit Manna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kale_R/0/1/0/all/0/1">Ruta Kale</a> Comets are the most primordial objects in our solar system which are made of icy bodies. Comets used to release gas and dust when it moves close to the Sun. The C/2020 F3 (NEOWISE) is a large periodic comet that is moving in a near-parabolic orbit. The C/2020 F3 (NEOWISE) is the brightest comet in the northern hemisphere after comet Hale-Bopp in 1997. Here we present the first interferometric high-resolution detection of the comet C/2020Read More →

Fractional Dark Energy. (arXiv:2101.05072v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Landim_R/0/1/0/all/0/1">Ricardo G. Landim</a> In this paper we introduce the fractional dark energy model, in which the accelerated expansion of the Universe is driven by a non-relativistic gas (composed by either fermions or bosons) with a non-canonical kinetic term. The kinetic energy is inversely proportional to the cube of the absolute value of the momentum for a fluid with equation of state parameter equal to minus one, and whose corresponding energy density mimics the one of the cosmological constant. In the general case, the dark energy equation of state parameter (times three) is precisely the exponent of the momentumRead More →

The PAU Survey: narrowband photometric redshifts using Gaussian processes. (arXiv:2101.03723v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Soo_J/0/1/0/all/0/1">John Y. H. Soo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joachimi_B/0/1/0/all/0/1">Benjamin Joachimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eriksen_M/0/1/0/all/0/1">Martin Eriksen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siudek_M/0/1/0/all/0/1">Ma&#x142;gorzata Siudek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alarcon_A/0/1/0/all/0/1">Alex Alarcon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabayol_L/0/1/0/all/0/1">Laura Cabayol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">Jorge Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casas_R/0/1/0/all/0/1">Ricard Casas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castander_F/0/1/0/all/0/1">Francisco J. Castander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_E/0/1/0/all/0/1">Enrique Fern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">Juan Garci&#xe1;-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaztanaga_E/0/1/0/all/0/1">Enrique Gaztanaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hildebrandt_H/0/1/0/all/0/1">Hendrik Hildebrandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoekstra_H/0/1/0/all/0/1">Henk Hoekstra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miquel_R/0/1/0/all/0/1">Ramon Miquel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_C/0/1/0/all/0/1">Cristobal Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_E/0/1/0/all/0/1">Eusebio S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serrano_S/0/1/0/all/0/1">Santiago Serrano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tallada_Crespi_P/0/1/0/all/0/1">Pau Tallada-Cresp&#xed;</a> We study the performance of the hybrid template-machine-learning photometric redshift (photo-$z$) algorithm Delight, which uses Gaussian processes, on a subset of the early data release of the Physics of the Accelerating Universe SurveyRead More →

Are extrasolar Einstein’s spinning tops habitable?. (arXiv:2012.14245v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Iorio_L/0/1/0/all/0/1">Lorenzo Iorio</a> Recently, the possibility that putative massive natural satellites (exomoons) of extrasolar Jupiter-like giant planets orbiting main sequence stars may be habitable has gained increasing attention. Typically, such an exomoon is expected to orbit its parent planet in the equatorial plane of the latter, with its spin $boldsymbol S$ aligned with its orbital angular momentum $boldsymbol L$ which, in turn, is parallel to the planetary spin $boldsymbol J$. If, in particular, the common tilt of such angular momenta to the satellite-planet ecliptic plane, assumed fixed, has certain values, the overall irradiation experienced by theRead More →

Directional detection of light dark matter from three-phonon events in superfluid $^4$He. (arXiv:2012.01432v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Caputo_A/0/1/0/all/0/1">Andrea Caputo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Esposito_A/0/1/0/all/0/1">Angelo Esposito</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Piccinini_F/0/1/0/all/0/1">Fulvio Piccinini</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Polosa_A/0/1/0/all/0/1">Antonio D. Polosa</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Rossi_G/0/1/0/all/0/1">Giuseppe Rossi</a> We present the analysis of a new signature for light dark matter detection with superfluid $^4$He: the emission of three phonons. We show that, in a region of mass below the MeV, the kinematics of this process can offer a way to reconstruct the dark matter interaction vertex, while providing background rejection via coincidence requirements and directionality. We develop all the necessary technology to deal with such an observable, and compute the associated differentialRead More →

Perseverance Begins its Science on Mars With a Laser zap Perseverance has already made its mark on scientific history by taking the first audio recording ever on Mars.  But the instrument with the microphone, known as the SuperCam, wasn’t done there.  It has plenty of other science to do, and recently it started running through some more preliminary tests.  One of those tests happened to involve blasting a rock with a laser – while taking an audio recording of it. SuperCam itself is the brainchild of scientists at Los Alamos National Laboratory and a consortium of European research universities with the French Centre National d’EtudesRead More →

B2 1420+32 is a changing-look blazar, study finds An international team of astronomers has performed multi-wavelength photometric and spectroscopic observations of a blazar known as B2 1420+32. The observational campaign found that the object exhibits a large scale spectral variability and is the so-called “changing-look” blazar. The findings are reported in a paper published March 15 on arXiv.org. phys.org Go to SourceRead More →

Correlations between H$alpha$ Equivalent Width and Galaxy Properties at $z = 0.47$: Physical or Selection-driven?. (arXiv:2103.10959v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Khostovan_A/0/1/0/all/0/1">Ali Ahmad Khostovan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malhotra_S/0/1/0/all/0/1">Sangeeta Malhotra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rhoads_J/0/1/0/all/0/1">James E. Rhoads</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harish_S/0/1/0/all/0/1">Santosh Harish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_C/0/1/0/all/0/1">Chunyan Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Junxian Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wold_I/0/1/0/all/0/1">Isak Wold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_Z/0/1/0/all/0/1">Zhen-Ya Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrientos_L/0/1/0/all/0/1">L. Felipe Barrientos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_A/0/1/0/all/0/1">Alicia Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_W/0/1/0/all/0/1">Weida Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Infante_L/0/1/0/all/0/1">Leopoldo Infante</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_L/0/1/0/all/0/1">Lucia A. Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pharo_J/0/1/0/all/0/1">John Pharo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valdes_F/0/1/0/all/0/1">Francisco Valdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walker_A/0/1/0/all/0/1">Alistair R. Walker</a> The H$alpha$ equivalent width (EW) is an observational proxy for specific star formation rate (sSFR) and a tracer of episodic star-formation activity. Previous assessments show that EW strongly anti-correlates with stellar mass as $M^{-0.25}$ similarRead More →