Comparison of the Short Gamma Ray Burst Host Galaxies of Gaia and VLBI-Gaia Data Release 2

Fong, W. et al. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. VIII. A comparison of short- duration burst with long- duration burst. Astrophys. J. Lett. 848 was published in L23.

Nugent, A. E. et al. Short GRB host galaxies II: a legacy sample of redshifts, stellar population properties, and implications for their neutron star merger origins. Preprints at arXiv.org.

Makhathini, S. et al. The panchromatic afterglow features the full uniform data set, modeling, comparison and implications. Astrophys. J. 922, 154 (2021).

Fender, R. in Compact Stellar X-ray Sources (eds Lewin, W. & van der Klis, M.) Cambridge Astrophysics Series, No. 39, 381–420 (Cambridge Univ. Press, 2006

Bellini, A., Anderson, J. & Bedin, L. R. Astrometry and photometry with HST WFC3. II. 10 filters of the UVIS channel have geometric-distortion corrected. There is a Publ. Astron. Soc. Pac. 123, 622 (2011).

Greisen, E. W. in Information Handling in Astronomy—Historical Vistas Astrophysics and Space Science Library Vol. 285 (ed. Heck, A.) 109–125 (Springer, 2003).

There are Systematics and Accuracy of VLBI Astrometry that are Comparison with Gaia Data Release 2. Astron. Astrophys. 634, A28 (2020).

Kovalev, Y. Y., Petrov, L. & Plavin, A. V. VLBI-Gaia offsets favor parsec-scale jet direction in active galactic nuclei. Astron. There are astrophys.

Petrov, L., Kovalev, Y. Y. & Plavin, A. V. An analysis of positions and motions of the Gaia DR2 with respect to the VLBI. The day was Mon. Not. R. Astron. Soc. 482, 3023–3031 (2019).

P. Charlot, et al. The third realization of the International Celestial Reference Frame by very long baseline interferometry. Astron. Astrophys. 644, A161 (2020).

J. S., Kulkarni, S. R. and S. G. were present. The observed offset distribution of gamma-ray bursts from their host galaxies: a robust clue to the nature of the progenitors. Astron. J. 123 came out in 2002.

Speagle’s package is a sampling package for estimating the effects of a number of factors. Mon. Not. R. Astron. 353, 347, and 3158 were published in 2020.

The Fermi GBM Team. Observation of GRB 211211A: SPI-ACS/INTEGRAL/NIR and observations of Swift-XRT

Soares-Santos, M. The Dark Energy Survey and The Dark Energy Camera GW-EM Collaboration et al. The LIGO/Virgo merger is an equivalent to the plutonium star merger. The optical counterpart was found using the dark energy camera. Astrophys. J. 848, L16 was published on July 16th.

The team is from the Fermi GBM Team. GRB 211211A: Fermi GBM observation. GRB Coordinates Network, Circular Service, No. 31210 (2021).

Nicholl, M. There are some constraints on the calculation of the state of a neutron star. Mon. Not. R. Astron. The paper reports on 3016–3032 (2021).

The NIR emission after the long duration GRB211212A: dust heating as an alternative to a kilonova was very strong. Preprint at https://arxiv.org/abs/2206.10710 (2022).

There are effects of r-process heating on fallback accretion in compact object mergers. Mon. Not. R. Astron. There was a report about this in “Soc 402, 2771-2-777”.

Adriani, O. et al. The International Space Station has a calorimetrics electron telescope that can measure the Cosmic-ray electron and positron spectrum from 11 GeV to 4.8 TeV. Phys. Rev. Lett. 120, 261102 (2018).

Minaev, P. & Pozanenko, A.; GRB IKI FuN. GRB 211211A: redshift estimation and SPI-ACS/INTEGRAL detection. GRB Coordinates Network, Circular Service, No. 31230 (2021).

Evans, P. A. The results of a complete sample of Swift-XRT observations were analyzed. The day was on Mon. Not. There is R. Astron. Soc. 397, 1177–1201 (2009).

Hook, I. M. The Gemini–North Multi-Object Spectrograph: performance in imaging, long-slit, and multi-object spectroscopic modes. Publ. Astron. Soc. 116, 423, 450 and 480 from 2004.

Labrie, K., Anderson, K., Cárdenes, R., Simpson, C. & Turner, J. E. H. DRAGONS – Data Reduction for Astronomy from Gemini Observatory North and South. There is a conference called the “asp conf.” Ser. 523 was published on March 28, 2019.

Lang, D., Hogg, D. W., Mierle, K., Blanton, M. & Roweis, S. Astrometry.net: blind astrometric calibration of arbitrary astronomical images. Astron. J. 139, 1782–1800 was published in 2010.

The reddening was measured with a telescope and recalibrating the sky. Astrophys. J. 99, 103 was published in 2011.

Willmer, C. N. A. et al. The Deep Evolutionary Exploratory Probe 2 galaxy redshift survey: the galaxy luminosity function to z ~ 1. Astrophys. J. 647, 853–873 (2006).

S. L and Finkelstein discuss their research. The evolution of the galaxy rest-frame ultraviolet luminosity function over the first two billion years. Astrophys. J. 760, 71.

Nugent, A. E. The distant, galaxy cluster environment of the short GRB 161104A at z ~ 0.8 and a comparison to the short GRB host population. Astrophys. J. 902, 54 (2020).

Wright, E. L. The initial on-orbit performance and mission description of the Wide-field Infrared Survey Explorer (WISE). Astron. J. 140 was written in 1868.

There is propagation of uncertainties in stellar population synthesis modeling. III. Model calibration, comparison, and evaluation. Astrophys. J. 712, 833, and 858 were published in 2010.

M.C., Daz and a few others collaborated on a project. Observations of the first electromagnetic counterpart to a gravitational-wave source by the TOROS collaboration. There are astrophys. L29 was published by J. 548, L 848.

Source: https://www.nature.com/articles/s41586-022-05390-w

Gravitational waves from the merger of two dead stars: puzzles and constraints on kilonova detection in two short GRBs at z 0.5

W., Dietrich, T., Margalit, B. and Metzger, B. D. There’s a debate on Mon. Not. R. Astron. Soc. 489, 91–96 (2019).

On August 17, 2017, two dead stars’ remnant cores collided into each other outside of our solar system. Known as a neutron star merger, they detected this event via ripples in spacetime—known as gravitational waves—and light produced by the resulting explosion. This was the first time that scientists had seen this type of event. The stars were between 1.1 and 1.6 times the mass of the Sun. Some of the heavier elements found in the universe, such as gold and Platinum, can be traced back to the collisions. More puzzles than answers was presented by the signals.

S. Khan and her friends, et al. There are waves from black-hole binaries. I. A phenomenological model for the advanced detector era. The Phys. Rev. D 93 was published on 2016-01-01.

High resolution numerical relativity simulations were used to create closed-form tidal approximants. Phys. Rev. D 96, 121501 (2017).

O’Connor, B. A tale of two mergers: constraints on kilonova detection in two short GRBs at z ~ 0.5. Mon. Not. R. Astron. Soc. 502, 1279–1298 (2021).

The SAO RAS optical observations are from GRB IKI FuN. There is a network and circular service.

A kilonova-like pair of neutron stars: Dr. Christopher Richardson and his assistant professor of physics and astronomy

Over time — that is, likely a couple billion years — the two neutron stars will merge and eventually explode in a kilonova, releasing heavy elements like gold into the universe.

There was a big flash of X-ray light from the same region in the sky where a hot, bright Be-type star was located.

The data was collected using a 1.5 meter telescope in northernChile as Astronomers were curious if the two could possibly be linked.

One of those interested in using this data to learn more about the star was Dr. Noel D. Richardson, now an assistant professor of physics and astronomy at Embry-Riddle Aeronautical University.

Clarissa Pavao approached Richardson while taking his astronomy class to ask if he had any projects she could work on to gain experience with astronomy research. Pavao learned how to clean up the data from the telescope in chile, after he shared the telescope data with her.

A star’s elements can be seen with a telescope, but disks of matter surround them, Pavao said. It’s difficult to see through all that stuff.

Source: https://www.cnn.com/2023/02/01/world/supernova-rare-star-pair-scn/index.html

A Rare Stellar Pair in the Circularly-Orbiting Binary CPD-29 2176 and Its Implications to the Formation of a Supernova

They were expecting something different. Typically, binary stars whirl around one another in an oval-shaped orbit. In CPD-29 2176, one star orbits the other in a circular pattern that repeats about every 60 days.

The two stars, a larger one and a smaller one, were whirling around one another in a very close orbit. Over time, the larger star had begun to shed its hydrogen, releasing material onto the smaller star, which grow from 8 or 9 times the mass of our sun to 18 or 19 times the mass of our sun, Richardson said. Our sun has a mass which is 333,000 times that of Earth.

The main star became smaller and smaller while building up the secondary star — and by the time it had exhausted all of its fuel, there wasn’t enough to create a massive, energetic supernova to release its remaining material into space.

“The star was so depleted that the explosion didn’t even have enough energy to kick (its) orbit into the more typical elliptical shape seen in similar binaries,” Richardson said.

The dense remnant of a pulsar that was left after the supernova is now in the path of a rotating massive star. The stellar pair will be in a stable configuration for between 5 and 7 million years. A disk of gas must be released to maintain balance due to the transfer of mass and momentum to the Be star.

The secondary star will burn through fuel and release more material like the first one did. The star system is able to release the material through space because it can’t easily pile it up on the neutron star. The secondary star will likely experience a similar lackluster supernova and turn into a neutron star.

Source: https://www.cnn.com/2023/02/01/world/supernova-rare-star-pair-scn/index.html

Stars and the Birth and Death of the Universe, Part I: Analysis and Future Prospects for HST and the Hubble Space Telescope

“Those heavy elements allow us to live the way that we do. For example, most gold was created by stars similar to the supernova relic or neutron star in the binary system that we studied. Richardson said that astronomy deepens our understanding of the world.

Pavao said we look back through time when we look at these objects. “We get to know more about the origins of the universe, which will tell us where our solar system is headed. We had the same elements as these stars when we were humans.

Richardson and Pavao also worked with physicist Jan J. Eldridge at the University of Auckland in New Zealand, an expert on binary star systems and their evolution. There are likely only 10 star models like the one in the study that exists in the entirety of the Milky Way, according to a review by Eldridge.

Next, the researchers want to work on learning more about the Be star itself, and hope to conduct follow-up observations using the Hubble Space Telescope. Pavao is working on space physics research using the new skills she has learned, as she sets her sights on graduating.

Forget archaeologists and their lost civilizations, or paleontologists with their fossils—astrophysicist Heloise Stevance studies the past on an entirely different scale. When astronomers catch a glimpse of an unusual signal in the sky, perhaps the light from a star exploding, Stevance takes that signal and rewinds the clock on it by billions of years. She uses stellar genealogy to look at the past lives of dead and dying stars. “There’s a lot of drama in the lives of stars,” she says.

Researchers don’t know how common these mergers are, and they can’t tell whether they are responsible for creating all the heavy elements in the universe, or just a fraction. However, if astrophysicists could observe more of these mergers, they could answer even deeper questions like how old the universe is. This is where stellar genealogy can help.

The work also describes interactions between the two stars before they burned out their fuel to become neutron stars. They started tens of millions of kilometers apart, which sounds far but is actually well under the distance between Earth and the Sun. Each star’s exterior was surrounded by gas known as a stellar envelope. The models of her team determined that at least twice, the outer gases of the two stars merged to become a single shared envelope.