vania-janet/multiturn-rag-retrieval-data huggingface dataset:
Astrophysics Science Division Colloquium Series Schedule: Spring 2024
Chandra & the SuperMassiveBlackHole - Galaxy Interaction
Giuseppina Fabbiano
Center for Astrophysics, Harvard & Smithsonian
Tuesday, Mar 5, 2024

Abstract
Launched from Cape Canaveral on July 23, 1999, Chandra is the NASA Great Observatory for the X-ray band. Now in its 25th year of operations, Chandra has revolutionized our view of the X-ray sky, thanks to its sub-arcsecond imaging and spectral capabilities. This talk will introduce Chandra and will then concentrate on Chandra's contributions to our understanding of one of the open mysteries of Astrophysics: "Feedback" - How is it that supermassive black holes (SMBH, with mass ~10 millions to billions of that of our Sun) in their Active Galactic Nucleus (AGN) phase interact with the billion times larger host galaxy and shape its evolution? Some form of "feedback" is needed to explain universe survey data and simulations, but observationally constraining its physical mechanisms is still an open field of research. Observing nearby AGN host galaxies with Chandra we have studied in detail the spatial and spectral properties of the AGN-host interaction, from spatial scales ranging from a few kiloparsecs (~1/10 of the radius of the Milky Way) to ~30 parsec (~3 times the size of the Orion Nebula). In these galaxies, we have found evidence for all four vectors of feedback: the photons emitted by the AGN (radiation), relativistic jets embedded in the host galaxy disk, and both nuclear winds and, most recently, very fast nuclear winds. These observations are pointing to a revision of the AGN standard model, one where interactions with the host interstellar medium and molecular clouds are important parts of the AGN phenomenon.

Resonant Evolution: How emergent dynamics have shaped the Milky Way
Kathryne J. Daniel
University of Arizona, Steward Observatory
Tuesday, Mar 12, 2024

Abstract
Dynamical resonances are essential to the evolution of disk galaxies. These resonances arise in the presence of massive structures, like Giant Molecular Clouds, spiral patterns and satellites, and reshape a galaxy as they diffuse, shepherd and rearrange stellar populations.
Imagine the Universe!
The emission lines result from ultraviolet light from the star being reprocessed in the ejected material.
BeppoSAX
A major satellite program of the Italian Space Agency with partcipation from the Netherlands Agency for Aerospace Programs. BeppoSAX operated from 1996 to 2002, and covered more than three decades of energy (from 0.1 to 300 keV) with relatively large effective area, medium energy resolution and imaging capabilities from 0.1 - 10 keV. Among BeppoSAX's claims to fame is its first detection of an afterglow from a gamma-ray burst in 1997. BeppoSAX was named after Italian physicist Giuseppe Occhialini, whose nickname was Beppo.

 Tell me more about BeppoSAX.

Big Bang
A widely accepted model of the Universe that assumes that the observed expansion of the Universe originated about 13.7 billion years ago, when the Universe was very hot and very dense. It successfully explains the cosmic microwave background and the ratio of hydrogen, helium, and other light elements, as well as the expansion of the Universe.
binary stars
Binary stars are two stars that orbit around a common center of mass. An X-ray binary is a special case where one of the stars is a collapsed object such as a white dwarf, neutron star, or black hole, and the separation between the stars is small enough so that matter is transferred from the normal star to the compact star star, producing X-rays in the process.

 Tell me about X-ray binary stars.
 Tell me more about X-ray binary stars.

black dwarf
A non-radiating ball of gas resulting from a white dwarf that has radiated all its energy.
black hole
An object whose gravity is so strong that not even light can escape from it.

 Tell me about X-rays from black holes.
 Tell me more about black holes.

black-hole dynamic laws; laws of black-hole dynamics

First law of black hole dynamics:
	For interactions between black holes and normal matter, the conservation laws of mass-energy, electric charge, linear momentum, and angular momentum, hold. This is analogous to the first law of thermodynamics.
	Second law of black hole dynamics:
Imagine the Universe!
The derived SI< unit of frequency, defined as a frequency of 1 cycle per second.
HST
Hubble Space Telescope
Hubble, Edwin P. (1889 - 1953)
American astronomer whose observations proved that galaxies are "island universes", not nebulae inside our own galaxy. His greatest discovery, called "Hubble's Law", was the linear relationship between a galaxy's distance and the speed with which it is moving. The Hubble Space Telescope is named in his honor.

 Show me a picture of Edwin Hubble!

Hubble constant; Ho (E.P. Hubble; 1925)
The constant which determines the relationship between the distance to a galaxy and its velocity of recession due to the expansion of the Universe. After many years in which the Hubble constant was only known to be somewhere between 50 and 100 km/s/Mpc, it has been determined to be 70 km/s/Mpc ± 7 km/s/Mpc by the Hubble Space Telescope's Key Project team. (Advances in cosmology have shown that since the Universe is self gravitating, Ho is not truly constant. Astronomers thus seek its present value.)
Hubble's law (E.P. Hubble; 1925)
A relationship between a galaxy's distance from us and its velocity through space. The farther away a galaxy is from us, the faster it is receding from us. The constant of proportionality is the Hubble constant, Ho, named after Edwin P. Hubble who discovered the relationship. Hubble's Law is interpreted as evidence that the Universe is expanding. 
Huygens, Christiaan (1629 - 1695)
A Dutch physicist who was the leading proponent of the wave theory of light. He also made important contributions to mechanics, stating that in a collision between bodies, neither loses nor gains ``motion'' (his term for momentum). In astronomy, he discovered Titan (Saturn's largest moon) and was the first to correctly identify the observed elongation of Saturn as the presence of Saturn's rings.

 Show me a picture of Christian Huygens!

hydrogen
The lightest and most abundant element. A hydrogen atom consists of one proton and one electron.
Galaxies Actively Forming in Early Universe Caught Feeding on Cold Gas - NASA Science
Galaxies Actively Forming in Early Universe Caught Feeding on Cold Gas - NASA Science

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Explore the Electromagnetic Spectrum | NASA Space Place – NASA Science for Kids
Explore the Electromagnetic Spectrum | NASA Space Place – NASA Science for Kids

magic-windows

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Earth
Sun
Solar System
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Science and Tech
Educators

chandra-x-ray-observatory

Explore the Electromagnetic Spectrum

Credit: NASA/JPL-Caltech
Explore the "Magic Windows" of the electromagnetic spectrum below!

Radio Waves

Credit: NASA/JPL-Caltech
Radio waves are very long and not very energetic. Radio waves can be from about the length of a football field up to 100 kilometers (60 miles) and more.Here we see a quasar (for "quasi-stellar object") through the Magic Radio Window. Quasars look a bit like stars but are very different in many ways. They are some of the most distant objects we see, and they put out great amounts of radio energy. Astronomers think they may be the centers of active galaxies that have supermassive black holes.
Like a radio telescope, this Magic Window sees radio objects in the sky, then a computer converts that energy to colors in the visible part of the spectrum that we can see.

Microwaves

Credit: NASA/JPL-Caltech
Microwaves are from about 1 millimeter (about the size of a sharp pencil point) to about 1 foot long.
This window shows us the microwave energy known as the cosmic background radiation. It is the "noise" left from shortly after the Big Bang that began the universe billions of years ago. The different colors represent very tiny differences in energy that eventually resulted in matter clumping together into galaxies and even bigger structures throughout the universe.
This information was gathered by the Cosmic Background Explorer spacecraft over 4 years in the early 1990's.

Infrared Waves

Credit: NASA/JPL-Caltech

Credit: NASA/JPL-Caltech

Infrared waves are about the length of a grain of sand.
Do you recognize the constellation Orion? If you could see Orion in the infrared part of the electromagnetic spectrum, this is what you would see. Most of the stars you normally see in Orion don't stand out in this wavelength.
Astrophysics Science Division Colloquium Series Schedule: Spring 2024
Comprised of 42 elements, each 6.1m in diameter, the ATA is the first instrument built from the ground up to perform the search for extraterrestrial intelligence (or SETI). Operating within the 1 to 12 GHz frequency spectrum, the ATA captures electromagnetic radiation, with its digitized data processed centrally in a dedicated signal processing cluster onsite. Observers can then access this data to perform a plethora of scientific investigations. This spans the study of the enigmatic Fast Radio Bursts, brief bursts of radio energy with elusive origins, to the exploration of slow transients like supernovae and tidal disruption events.
In this talk, I will give an overview of the historical significance of radio astronomy emphasizing its pivotal role in astrophysics, and then delve into the ongoing upgrades of the ATA, elucidating the telescope's potential to advance both slow and fast transient science and the exciting prospects it holds for future discoveries.

Tell-tale electromagnetic signatures of massive black hole binaries
Jordy Davelaar
CCA/Flatiron Institute and Columbia University
Tuesday, Apr 2, 2024

Abstract
Due to galactic mergers, massive black hole binaries are thought to reside in the cores of numerous galaxies. As the massive black holes migrate inwards, they will eventually emit gravitational waves, which are expected to be detected by LISA. A critical component to understanding where and how black holes merge and how they shape galactic evolution is host galaxy identification, which relies on electromagnetic (EM) observations. In my talk, I will show two novel tell-tale EM signatures that would provide strong evidence for a black hole binary before or during a merger. The first is when the binary is seen close to edge on; in that case, the binary produces self-lensing flares (SLFs) when one of the black holes moves in front of the background black hole. This causes the emission to be gravitationally lensed. This signal can additionally hold information on the size and shape of the emission morphology of the lensed black hole. Secondly, I will argue that when the binary is close to merger, the accretion is disrupted, turning the binary X-ray dark.
Astrophysics Science Division Colloquium Series Schedule: Spring 2024
I will show how using spectroscopic observations of star clusters and their nearby gas allows us to observe the chemical evolution of galaxies through a much larger window in both space and time. Lastly, I will present some of the most recent results from our JWST program dedicated to dissect a key ingredient in the recipe for star formation: molecular gas. I will close with a brief discussion on the implications these data have in the understanding of the processes that drive the evolution of galaxies.

Uncovering the Elusive Origin of Fast Radio Bursts and other Radio Transients
Tarraneh Eftekhar
Northwestern University
Tuesday, May 7, 2024

Abstract
The last decade of investigations into the extragalactic radio sky has led to a paradigm shift, with all-together new and uncharacterized populations of radio transients emerging for the first time. Upgrades in multiple fast radio burst (FRB) experiments have led to the first samples of precisely localized events, enabling host galaxy associations and detailed observations of the immediate environments surrounding FRBs. Such observations play a key role in elucidating the stellar populations that give rise to FRB progenitors. In this talk, I will review our current knowledge of FRB progenitors based on the properties of a small, but growing sample of host galaxies, and I will outline major follow-up efforts to build the first statistically meaningful sample of FRB hosts. The localizations of two repeating FRBs to dwarf galaxies and their coincidence with persistent radio sources — coupled with detections of long-lived radio transients in dwarf galaxies --further implicate an entirely new population of radio sources on the sky. I will discuss our large-scale effort to uncover this unique population for the first time. Finally, I will discuss prospects for opening a new window into the transient sky at millimeter wavelengths.

Deep Reconnaissance of Exoplanet Atmospheres with JWST
Nikole Lewis
Cornell University
Tuesday, May 14, 2024

Abstract
With JWST a new window into exoplanet atmospheres is now wide open. Cycle 1 JWST observations of exoplanet hosting systems have already proven the power of this observatory to provide new and transformational insights into exoplanet atmospheres.
Imagine the Universe!
proton 
A particle with a positive charge commonly found in the nucleus of atoms.
protostar
Very dense regions (or cores) of molecular clouds where stars are in the process of forming.
Ptolemy (ca. 100-ca. 170)
A.k.a. Claudius Ptolemaeus. Ptolemy believed the planets and Sun to orbit the Earth in the order Mercury, Venus, Sun, Mars, Jupiter, Saturn. This system became known as the Ptolemaic system and predicted the positions of the planets accurately enough for naked-eye observations (although it made some ridiculous predictions, such as that the distance to the moon should vary by a factor of two over its orbit). He authored a book called Mathematical Syntaxis (widely known as the Almagest). The Almagest included a star catalog containing 48 constellations, using the names we still use today.

 Show me a picture of Ptolemy!

pulsar
A rotating neutron star which generates regular pulses of radiation. Pulsars were discovered by observations at radio wavelengths but have since been observed at optical, X-ray, and gamma-ray energies.

 Tell me about pulsars!
 Tell me more about pulsars!

PVO
Pioneer Venus Orbiter

 Tell me more about PVO

Q
quasar
An enormously bright object at the edge of our universe which emits massive amounts of energy. In an optical telescope, they appear point-like, similar to stars, from which they derive their name (quasar = quasi-stellar). Current theories hold that quasars are one type of AGN.
quasi-stellar source (QSS)
Sometimes also called quasi-stellar object (QSO); A stellar-appearing object of very large redshift that is a strong source of radio waves; presumed to be extragalactic and highly luminous.
R
radial velocity
The speed at which an object is moving away or toward an observer. By observing spectral lines, astronomers can determine how fast objects are moving away from or toward us; however, these spectral lines cannot be used to measure how fast the objects are moving across the sky.
radian; rad
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Life in the UniverseStarsGalaxiesBlack HolesThe Big BangDark Matter &amp; Dark EnergyThe Solar System The SunMercuryVenusEarthThe MoonMarsJupiterSaturnUranusNeptunePluto &amp; Dwarf PlanetsAsteroids, Comets &amp; MeteorsThe Kuiper BeltThe Oort CloudSkywatchingEspañol CienciaAeronáuticaCiencias TerrestresSistema SolarUniversoScience All NASA ScienceEarth SciencePlanetary ScienceAstrophysics & Space ScienceThe Sun & HeliophysicsBiological & Physical SciencesLunar ScienceCitizen ScienceAstromaterialsAeronautics ResearchHuman Space Travel ResearchExploreSearchSubmitNews & EventsMultimediaNASA+HomeUniversoGlosario de la NASAInicioCiencias terrestresCambio climáticoSistema solarUniversoGente de la NASAAcerca de CienciaExplore This SectionInicioCiencias terrestresCambio climáticoSistema solarUniversoGente de la NASAAcerca de Ciencia1 min de lecturaGlosario de la NASANoelia GonzálezMay 06, 2024ArtículoContentsEpisodios del Glosario de la NASA:Bienvenidos al Glosario de la NASA, en donde exploramos términos de ciencias espaciales y de la Tierra a través de videos cortos. ¿Sientes curiosidad por los fenómenos que ocurren en nuestro planeta natal y en el resto del universo? ¡Has llegado al lugar indicado! Echa un vistazo a nuestra creciente lista de episodios y aprende sobre los términos que más te interesen.Episodios del Glosario de la NASA:¿Qué es una fusión de galaxias?
Astrophysics Science Division Colloquium Series Schedule: Spring 2024
Although FRBs are likely associated with neutron stars, they appear to occur in a remarkable diversity of environments. Understanding the formation of FRB sources is thus intertwined with problems in neutron-star formation. FRBs additionally form exquisite tracers of the contents and physical conditions of the otherwise "missing" baryons along their sightlines. The Deep Synoptic Array (DSA-110) radio telescope, now fully operational at Caltech's Owens Valley Radio Observatory, is discovering and pinpointing FRBs to host galaxies at a world-leading rate. I will present results from the first DSA-110 FRB sample. The host-galaxy properties of the sample shed new light on the origins of FRBs. DSA-110 discoveries are, for the first time, sensitively determining the split between the cosmic baryon contents around and in between galaxies. Polarization data probe the characteristic magnetizations along FRB sightlines, predominantly in the host-galaxy interstellar medium. I will conclude with an outlook towards the use of several thousands of localized FRBs with the DSA-2000 for tomography of the intergalactic medium, and to shed fresh light on cosmological problems.

Recent Colloquia Schedules

2023: Fall, Spring
2022: Fall, Summer, Spring
2021: Fall, Spring

All Past ASD Colloquia Schedules