Observational Limits on the Early-time Dust Mass in SN 1987A

Abstract In recent years, dust masses of a few tenths of a solar mass have been found in the expanding ejecta of a number of core-collapse supernovae. How dust forms in such quantities remains poorly understood; theories of dust formation predict lower total masses and much faster formation rates than observations imply. One suggestion to reconcile observations and theory was made by Dwek et al., who proposed that the dust forms very rapidly, and because of its optical depth, is not initially observationally detectable, only being gradually revealed as the ejecta expand. Observational dust masses at early times would then only be lower limits. Using a large grid of radiative transfer models covering dust masses from 10−4 to 1 M ⊙ to calculate both the spectral energy distribution and the emission line profiles from clumpy dust shells, we show that this cannot be the case. Some clump distributions allow dust masses of ∼0.01 M ⊙ to be concealed in clumps and still predict an SED consistent with the observations. However, these geometries predict emission line profiles that are inconsistent with the observations. Similarly, clump geometries that reproduce the observed emission line profiles with dust masses >0.01 M ⊙ do not reproduce the SED. However, models with ∼10−3 M ⊙ of amorphous carbon can reproduce both the SED and the emission line profiles. We conclude that no large masses of dust can be hidden from view in the ejecta of SN 1987A at early epochs, and that the majority of dust must thus have formed at epochs >1000 days.

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The Hα line emission of the Be star β Psc: the last 40 yr

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2789 ◽

2020 ◽

Vol 501 (1) ◽

pp. 747-755

Author(s):

Ronaldo S Levenhagen ◽

Marcos P Diaz ◽

Eduardo B Amôres ◽

Nelson V Leister

Keyword(s):

Additional Data ◽

State Of The Art ◽

Spectral Energy Distribution ◽

Line Emission ◽

Spectral Energy ◽

Line Profiles ◽

Gas Density ◽

Geometric Deformation ◽

Be Star ◽

Effects Of Rotation

ABSTRACT A study on the photosphere and disc of the Be star β Psc is presented. We recover almost 40 yr of high-resolution spectroscopic observations and additional data gathered from the BeSS data base. We evaluate the photospheric parameters from the spectral energy distribution (SED) and fittings of state-of-the-art non-LTE model atmospheres to observed helium, carbon, silicon, and magnesium line profiles. Our models include the stellar geometric deformation as well as the co-latitude dependence of temperature and gravity, aiming to derive the effects of rotation on the stellar parameters. We estimate the circumstellar disc parameters from the fitting of models assuming different disc properties, namely its radius and gas density profile. The disc inclination angle i is constrained from the fittings of He i 4471 Å, Mg ii 4481 Å, C ii 4267 Å, and Si ii 4128, 4132 Å lines with gravity darkened models. Our findings, based on model fittings, suggest that during the last 40 yr, the disc radius changed within the interval 5.5 ≤ Rd ≤ 7.8 $R/R_{*}\,$, the disc base gas density within 5 × 10−13 ≤ ρ ≤ 1 × 10−12 g cm−3, while the radial power-law density index m assumed values between 2.0 and 2.3. These results are in agreement with recent works dealing with spectroscopic and interferometric measurements of this object.

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SNR G39.2−0.3, an hadronic cosmic rays accelerator

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2045 ◽

2020 ◽

Vol 497 (3) ◽

pp. 3581-3590

Author(s):

Emma de Oña Wilhelmi ◽

Iurii Sushch ◽

Robert Brose ◽

Enrique Mestre ◽

Yang Su ◽

...

Keyword(s):

Magnetic Field ◽

Cosmic Rays ◽

Supernova Remnants ◽

Gamma Ray ◽

Spectral Energy Distribution ◽

Galactic Cosmic Rays ◽

Spectral Energy ◽

Core Collapse ◽

Heavy Nuclei ◽

The Rich

ABSTRACT Recent results obtained with gamma-ray satellites have established supernova remnants as accelerators of GeV hadronic cosmic rays. In such processes, CRs accelerated in SNR shocks interact with particles from gas clouds in their surrounding. In particular, the rich medium in which core-collapse SNRs explode provides a large target density to boost hadronic gamma-rays. SNR G39.2–0.3 is one of the brightest SNR in infrared wavelengths, and its broad multiwavelength coverage allows a detailed modelling of its radiation from radio to high energies. We reanalysed the Fermi-LAT data on this region and compare it with new radio observations from the MWISP survey. The modelling of the spectral energy distribution from radio to GeV energies favours a hadronic origin of the gamma-ray emission and constrains the SNR magnetic field to be at least ∼100 µG. Despite the large magnetic field, the present acceleration of protons seems to be limited to ∼10 GeV, which points to a drastic slow down of the shock velocity due to the dense wall traced by the CO observations, surrounding the remnant. Further investigation of the gamma-ray spectral shape points to a dynamically old remnant subjected to severe escape of CRs and a decrease of acceleration efficiency. The low-energy peak of the gamma-ray spectrum also suggests that that the composition of accelerated particles might be enriched by heavy nuclei which is certainly expected for a core-collapse SNR. Alternatively, the contribution of the compressed pre-existing Galactic cosmic rays is discussed, which is, however, found to not likely be the dominant process for gamma-ray production.

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PRINCIPAL COMPONENT ANALYSIS OF THE SPECTRAL ENERGY DISTRIBUTION AND EMISSION LINE PROPERTIES OF RED 2MASS ACTIVE GALACTIC NUCLEI

The Astrophysical Journal ◽

10.1088/0004-637x/692/2/1180 ◽

2009 ◽

Vol 692 (2) ◽

pp. 1180-1189 ◽

Cited By ~ 26

Author(s):

Joanna Kuraszkiewicz ◽

Belinda J. Wilkes ◽

Gary Schmidt ◽

Paul S. Smith ◽

Roc Cutri ◽

...

Keyword(s):

Principal Component Analysis ◽

Energy Distribution ◽

Emission Line ◽

Active Galactic Nuclei ◽

Spectral Energy Distribution ◽

Galactic Nuclei ◽

Principal Component ◽

Component Analysis ◽

Spectral Energy

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A Deep JI Survey of the Pleiades for Freely-Floating Superplanets and Brown Dwarfs at the Deuterium Burning Limit

Symposium - International Astronomical Union ◽

10.1017/s0074180900210553 ◽

2003 ◽

Vol 211 ◽

pp. 185-186

Author(s):

M. J. Schwartz ◽

E. E. Becklin ◽

B. Zuckerman

Keyword(s):

Energy Distribution ◽

Proper Motion ◽

Near Infrared ◽

Profile Analysis ◽

Spectral Energy Distribution ◽

Brown Dwarfs ◽

Spectral Energy ◽

Preliminary Results ◽

Methane Absorption ◽

Lower Limits

We present preliminary results from a deep near-infrared J-band and I-band photometric survey of the Pleiades for freely-floating superplanets and brown dwarfs (BD) near the deuterium burning limit (DBL). With limiting magnitudes of J=20.5 and I=23.5, we have selected candidate Pleiads on the basis of evolutionary tracks, color-magnitudes, and I-J color lower limits (non-detections at deep I-band). Likelihoods of membership will be ultimately determined by a combination of image profile analysis, spectral energy distribution, proper motion, and low-resolution measurements of near-infrared water and/or methane absorption slopes. If confirmed, our faintest candidates are predicted to have made the transition from L to T spectral types with temperatures down to 820 K, and masses approaching 10 MJup.

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Properties of gamma-ray decay lines in 3D core-collapse supernova models, with application to SN 1987A and Cas A

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa736 ◽

2020 ◽

Vol 494 (2) ◽

pp. 2471-2497 ◽

Cited By ~ 5

Author(s):

A Jerkstrand ◽

A Wongwathanarat ◽

H-T Janka ◽

M Gabler ◽

D Alp ◽

...

Keyword(s):

Gamma Ray ◽

Radioactive Decay ◽

Supernova Explosion ◽

3D Models ◽

Core Collapse ◽

Line Profiles ◽

Sn 1987A ◽

And Shifts ◽

Cas A ◽

Explosive Burning

ABSTRACT Comparison of theoretical line profiles to observations provides important tests for supernova explosion models. We study the shapes of radioactive decay lines predicted by current 3D core-collapse explosion simulations, and compare these to observations of SN 1987A and Cas A. Both the widths and shifts of decay lines vary by several thousand kilometres per second depending on viewing angle. The line profiles can be complex with multiple peaks. By combining observational constraints from 56Co decay lines, 44Ti decay lines, and Fe IR lines, we delineate a picture of the morphology of the explosive burning ashes in SN 1987A. For MZAMS = 15−20 M⊙ progenitors exploding with ∼1.5 × 1051 erg, ejecta structures suitable to reproduce the observations involve a bulk asymmetry of the 56Ni of at least ∼400 km s−1 and a bulk velocity of at least 1500 km s−1. By adding constraints to reproduce the UVOIR bolometric light curve of SN 1987A up to 600 d, an ejecta mass around 14 M⊙ is favoured. We also investigate whether observed decay lines can constrain the neutron star (NS) kick velocity. The model grid provides a constraint VNS > Vredshift, and applying this to SN 1987A gives a NS kick of at least 500 km s−1. For Cas A, our single model provides a satisfactory fit to the NuSTAR observations and reinforces the result that current neutrino-driven core-collapse SN models achieve enough bulk asymmetry in the explosive burning material. Finally, we investigate the internal gamma-ray field and energy deposition, and compare the 3D models to 1D approximations.

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Properties of LBGs with [OIII] detection at z ∼ 3.5

Astronomy and Astrophysics ◽

10.1051/0004-6361/201935975 ◽

2019 ◽

Vol 631 ◽

pp. A123 ◽

Cited By ~ 1

Author(s):

Fang-Ting Yuan ◽

Denis Burgarella ◽

David Corre ◽

Veronique Buat ◽

Médéric Boquien ◽

...

Keyword(s):

Physical Properties ◽

Emission Line ◽

Near Infrared ◽

Spectral Energy Distribution ◽

Formation Rate ◽

Line Emission ◽

Stellar Mass ◽

Spectral Energy ◽

Emission Data ◽

The Impact

Context. Nebular emission lines are critical to measure physical properties in the ionized gas (e.g., metallicity, the star formation rate, or dust attenuation). They also account for a significant fraction of broadband fluxes, in particular at the highest redshifts, and therefore can strongly affect the determination of other physical properties, such as the stellar mass, which are crucial in shaping our understanding of galaxy formation and evolution. Aims. We investigate a sample of 51 Lyman break galaxies at 3.0 < zspec < 3.8 with detected [OIII] line emissions and estimated the physical properties of these galaxies to examine the impact of including nebular emission data in the Spectral energy distribution (SED) fitting. Methods. We used the Code Investigating GALaxy Emission (CIGALE) to fit the rest-frame ultraviolet-to-near-infrared SEDs of these galaxies and their emission line data simultaneously. We ran CIGALE with and without the nebular model or the emission line data, and compare the results to show the importance of including the nebular emission line data in the SED fitting. Results. We find that without the nebular model, the SED fitting overestimates the stellar mass due to the strong [OIII] lines that are redshifted to the Ks-band, which is consistent with previous results. The emission line data are necessary to constrain the nebular model in the SED fitting. We examine the Ks-band excess, which is mostly used to estimate the emissions of the [OIII]+Hβ lines when there is no spectral data, and we find that the estimation and observation are statistically consistent. However, the difference can reach up to more than 1 dex in some catastrophic cases, which shows the importance of obtaining spectroscopic measurements for these lines. We also estimate the equivalent width of the Hβ absorption and find it negligible compared to the Hβ emission. Conclusions. Line emission is important to constrain the nebular models and to obtain reliable estimates of the physical properties of galaxies. These data should be taken into account in the SED fitting.

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The circumstellar environment of the FS CMa star IRAS 00470+6429

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311010830 ◽

2010 ◽

Vol 6 (S272) ◽

pp. 384-385

Author(s):

Alex C. Carciofi ◽

Anatoly S. Miroshnichenko ◽

Jon E. Bjorkman

Keyword(s):

Main Sequence ◽

Spectral Energy Distribution ◽

Spectral Energy ◽

Line Profiles ◽

Polar Wind ◽

Strong Emission ◽

Novel Approach ◽

Consistent Solution ◽

Dust Destruction ◽

Circumstellar Environment

AbstractFS CMa type stars are a recently described group of objects with the B[e] phenomenon that exhibit strong emission-line spectra and strong IR excesses. In this paper we report the first attempt for a detailed modeling of IRAS 00470+6429, for which we have the best set of observations. Our modeling is based on two key assumptions: the star has a main-sequence luminosity for its spectral type (B2) and that the circumstellar (CS) envelope is bimodal, composed of a slowly outflowing disk-like wind and a fast polar wind. Both outflows are assumed to be purely radial. We adopt a novel approach to describe the dust formation site in the wind that employs timescale arguments for grain condensation and a self-consistent solution for the dust destruction surface. With the above assumptions we were able to reproduce satisfactorily many observational properties of IRAS 00470+6429, including the HI line profiles and the overall shape of the spectral energy distribution.

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A search for radio afterglows from gamma-ray bursts with the Australian Square Kilometre Array Pathfinder

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab326 ◽

2021 ◽

Vol 503 (2) ◽

pp. 1847-1863

Author(s):

James K Leung ◽

Tara Murphy ◽

Giancarlo Ghirlanda ◽

David L Kaplan ◽

Emil Lenc ◽

...

Keyword(s):

Gamma Ray ◽

Phase 1 ◽

Spectral Energy Distribution ◽

Early Time ◽

Gamma Ray Bursts ◽

Spectral Energy ◽

Density Parameter ◽

Square Kilometre Array ◽

Optical Images ◽

Celestial Sphere

ABSTRACT We present a search for radio afterglows from long gamma-ray bursts using the Australian Square Kilometre Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, covering the entire celestial sphere south of declination +41○, and three epochs of the Variables and Slow Transients Pilot Survey (Phase 1), covering ∼5000 square degrees per epoch. The observations we used from these surveys spanned a nine-month period from 2019 April 21 to 2020 January 11. We cross-matched radio sources found in these surveys with 779 well-localized (to ≤15 arcsec) long gamma-ray bursts occurring after 2004 and determined whether the associations were more likely afterglow- or host-related through the analysis of optical images. In our search, we detected one radio afterglow candidate associated with GRB 171205A, a local low-luminosity gamma-ray burst with a supernova counterpart SN 2017iuk, in an ASKAP observation 511 d post-burst. We confirmed this detection with further observations of the radio afterglow using the Australia Telescope Compact Array at 859 and 884 d post-burst. Combining this data with archival data from early-time radio observations, we showed the evolution of the radio spectral energy distribution alone could reveal clear signatures of a wind-like circumburst medium for the burst. Finally, we derived semi-analytical estimates for the microphysical shock parameters of the burst: electron power-law index p = 2.84, normalized wind-density parameter A* = 3, fractional energy in electrons ϵe = 0.3, and fractional energy in magnetic fields ϵB = 0.0002.

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