Astrophysics Colloquium Archived Talks
2022-2023 archived Astrophysics Colloquium
2021-2022 archived Astrophysics Colloquium
2020-2021 archived Astrophysics Colloquium
Spring 2023
April 5, Anna Rosen (University of California, San Diego)
A Massive Star is Born: How Stellar Feedback Limits Accretion onto Massive Stars
Abstract: Massive stars play an essential role in the Universe. They are rare, yet the energy and momentum they inject into the interstellar medium (ISM) with their intense radiation fields and fast, isotropic radiatively-driven winds dwarfs the contribution by their vastly more numerous low-mass cousins. This stellar feedback influences star and galaxy formation, and drives the dynamical and chemical evolution of galaxies. Massive stars form from the gravitational collapse of magnetized, dense, and turbulent molecular gas located within Giant Molecular Clouds (GMCs). Feedback from massive stars’ radiation fields, collimated protostellar outflows, and stellar winds may limit their growth by accretion, necessitating detailed radiation magnetohydrodynamic (RMHD) simulations to understand how these processes may impact their formation. In this talk, I will present results from a series of RMHD simulations modeling the formation of massive stars and show that stellar feedback can quench accretion onto ~30 Msun stars that form in isolation. My results imply that stars more massive than this must form via large-scale, high ram-pressure dynamical inflows within GMCs, consistent with observations. This highlights the need for future studies to follow the gravitational collapse of GMCs in order to trace large-scale inflows to the birth sites of massive stars.
April 12, Ylva Goetberg (Carnegie)
The Discovery and Properties of Binary-stripped Helium Stars
Abstract: Massive stars stripped of their H-rich envelopes through mass transfer or common envelope ejection are thought to be the main progenitors of H-poor supernovae, to emit large amounts of hard ionizing radiation, and to constitute two necessary steps in the binary evolution pathways towards compact objects merging in gravitational wave events. Despite their importance, these stripped helium stars have remained elusive.
With new UV photometry combined with optical magnitudes, and follow-up optical spectroscopy, we identified a first sample of dozens of such stripped star systems in the Magellanic Clouds. We obtain estimates for their stellar parameters by fitting their optical spectra to a newly computed grid of helium star atmosphere models. Aligned with theoretical expectations, we find that stripped stars are hot (Teff~50-100 kK), compact (log g ~ 5), He-rich (Y_surf ~0.6-1), and H-poor (X_surf ~0-0.4). Furthermore, by matching the spectroscopic fits with the photometrical data, we find small radii (~1 Rsun), a range of luminosities (L ~ 1,000-100,000 Lsun), and masses that are sufficient to lead to core-collapse (~2-8 Msun). There are strong indications that the stellar winds are surprisingly weak, suggesting that binary-stripped helium stars are the main responsible for both IIb and Ib supernovae.
Apart from providing an observational anchor for both binary evolution models and simulations of common envelope ejection, this sample of stars prove that the full mass range of helium stars exists, forming a bridge between subdwarfs and Wolf-Rayet stars.
April 19, Lee Armus (Caltech/IPAC)
Using JWST to Study Local Luminous Infrared Galaxies: Early Release Science
Abstract: Through a combination of greatly enhanced sensitivity, together with spatial and spectral resolution, JWST is poised to transform our understanding of galactic evolution, providing a detailed look at the physics of star formation and black hole growth in nearby and distant galaxies. In Early Release Science program 1328, we are observing four nearby, Luminous Infrared Galaxies (LIRGs) selected from the Great Observatories All-sky LIRG Survey (GOALS) with NIRSPEC, NIRCAM and MIRI. These observations are generating a rich dataset for understanding the dynamics and energetics of the ISM on scalesof ~100pc in the nuclei of local LIRGs. I will describe our initial results, and prospects for future observations of dusty, merging galaxies with JWST.
April 26, Erica Nelson (CU Boulder)
The remarkable power of JWST to revolutionize our understanding of galaxy formation
Abstract: The launch and commissioning of the James Webb Space Telescope is ushering in a new era in our understanding of our cosmic origins. Galaxies are a fundamental building block of the universe, yet how they formed has remained enigmatic owing to our inability to observe them at early cosmic times. In just the first eight months of data, JWST is already revolutionizing our understanding of the early universe by allowing us to detect and resolve early galaxies at infrared wavelengths. In this talk, I will discuss some of the results that have come out of our work with JWST and their impact on our understanding of the formation and evolution of galaxies. This includes the discovery of candidate galaxies so old and massive they should not exist, the surprising shapes of HST-dark galaxies, and a new method for measuring kinematics that has revealed a monstrous spinning disk 1 billion years after the big bang. The first spatially-resolved infrared look at distant galaxies has revealed that our previous understanding of the emergence of galactic structure was faulty and requires a next-generation set of tools, which we are building. I’ll conclude with a discussion of where the field is moving and the rich discovery space in this new era of extragalactic astrophysics.
May 3, Giacomo Fragione (NU)
HIERARCHICAL BLACK HOLE MERGERS: A MULTI-BAND OPPORTUNITY FOR GRAVITATIONAL WAVES
Abstract: With about a hundred binary black hole (BBH) mergers detected via gravitational wave emission, our understanding of the darkest objects in the Universe has seen unparalleled steps forward compared to previous decades. While most of the events are expected to consist of first-generation BHs formed from the collapse of massive stars, others might be of a second or higher generation, containing the remnants of previous BH mergers. A fundamental limit for hierarchical mergers comes from the recoil kick imparted to merger remnants, which could result in the ejection from the host star cluster. However, hierarchical mergers can build up massive BHs and even form intermediate-mass black holes if the host cluster is massive and dense enough, as in nuclear star clusters and the most massive globular clusters. With their distinctive signatures of higher masses and spins, hierarchical mergers offer an unprecedented opportunity to learn about the densest systems in our Universe and to shed light on the elusive population of intermediate-mass black holes. The next years may bring hundreds of detections from hierarchical mergers with multi-band events chirping from space-based to ground-based detectors, promising a spectacular range of new science from stellar evolution to cosmology.
May 10, Merav Opher (BU)
The Sun's Trajectory in the Last 10 Million years and possible terrestrial implications on Climate and Biological Evolution
Abstract: Until recently the primary focus with respect to astronomical impacts on Earth’s climate and biota have centered around those arising from changes in the tilt of the Earth axis, spin and rotation, which not only drive seasonal change but are also implicated in shifts between arid and wet climatic regimes over periods ≥ 10,000 years, due to changes in solar insolation. The Sun moves large distances (~19pc/Myr) through the quite variable Interstellar Medium. There is geological evidence from 60Fe and 244Pu isotopes that Earth received interstellar material about 2-3 Myr ago and 7 Myr ago. These isotopes were interpreted evidence for a nearby supernova, however that has been cast into doubt. In this talk I will discuss our new research indicating the encounter of Earth with massive cold cloud in Local Ribbon of Cold Clouds, 3 Myr ago and with the edge of the Local Bubble 7 Myr ago. Both encounters shrinked the Sun’s protective bubble—the heliosphere—to within Earth’s orbit exposing Earth to a cold dense interstellar medium. Such scenario should be discussed in context with other ones proposed to explain the cooling seen by Oxygen isotopes measured in deep sea Foraminifera. I will discuss the possible terrestrial consequences to climate and to biological evolution. The exposure to a cold dense interstellar medium has implications on climate and increase radiation. Increased radiation alone could have effects on climate, organismal mutation rates, aging, and extinction rates, and thus broad patterns of diversification.
May 17, Josh Winn (Princeton)
Five Years of TESS
Abstract: The Transiting Exoplanet Survey Satellite (TESS) is NASA's ongoing mission to discover planets outside the solar system, and more generally, to explore the bright and time-variable sky. TESS uses four 10cm optical telescopes to perform precise time-series photometry over wide fields of view. In the five years since it was launched, TESS has covered nearly the entire sky, leading to the confirmation of 330 new planets and the identification of about 6000 planet candidates that are being followed up by ground-based observers. The initial goal of the TESS Mission -- to detect 50 planets smaller than Neptune and measure their masses -— was achieved in 2021, and now TESS is in an Extended Mission with broader goals. I will review the history of TESS since its inception in 2006, and the most important and interesting results that have been achieved thus far. I will also describe the characteristics of TESS data and how to use the data in your own research.
May 24, Andrew Howard (Caltech)
The Keck Planet Finder
Abstract: The Keck Planet Finder (KPF) is a new precision radial velocity instrument for the W. M. Keck Observatory that is designed to measure radial velocities with a precision of 30 cm/s to search for and characterize extrasolar planets. KPF achieved “first light” on the 10-m Keck I Telescope last fall and is starting science observations now that will push the frontier of studies of extrasolar planets. The core spectrometer in KPF covers visible wavelengths (445-870 nm) with a resolving power of 95,000. KPF’s design uses several novel techniques including a low thermal expansion material (Zerodur) in the spectrometer, an optical fiber system that slices and homogenizes the light entering the spectrometer, and a separate spectrometer at UV wavelengths to capture the Calcium H&K lines. This talk will tell the story of how KPF came to be, discuss its current status and recent results, and look forward to a path of discovery and continued improvement that has a goal of 10 cm/s precision and sensitivity to Earth-twin planets orbiting nearby stars.
May 31, Darach Watson (DAWN/University of Copenhagen)
The origin of the rapid neutron capture elements in neutron star mergers
Abstract: The processes that create the elements that make up the periodic table were laid down theoretically in the late 1950s, but the cosmic forges that actually carry out these processes have been more difficult to identify. The rapid (r) neutron capture process creates half of all the elements heavier than iron and the bulk of the heaviest elements, including almost all gold, platinum, and uranium. Its site is currently a major source of debate. I present spectroscopic evidence for the creation of r-process elements in the merger of two neutron stars, proving that such mergers do create large quantities of heavy elements and that neutron stars are composed of neutron-rich matter, a fact not spectroscopically demonstrated until now. I will also discuss constraints on the geometry of the merger from the spectra which pose severe challenges to neutron star merger model simulations and indicate how neutron star mergers can be used to measure the expansion rate of the universe with good accuracy Finally, I point the way to the future of neutron star merger studies at optical and near-infrared wavelengths.
Winter 2023
January 18, Ryan Sanders (UC Davis)
Insights into high-redshift galaxy formation and growth from chemical abundance measurements
Abstract: A key goal of galaxy evolution studies is to understand how galaxies form and grow over time. Our current theoretical picture of this process includes the accretion of gas from the intergalactic medium, converting gas into stars inside the interstellar medium (ISM), and energetic feedback from stellar evolutionary processes (e.g., supernovae) or accreting supermassive black holes that injects energy into the ISM and can drive large-scale outflows that eject gas from the galaxy. We can constrain the parameters of this cycle of baryons into, through, and out of galaxy disks using measurements of gas-phase chemical abundances that encode information about the strength of inflows and outflows as well as the star formation history. I will present new insights into high-redshift galaxy formation and gas flows based on new constraints on metallicity scaling relations including the mass-metallicity relation, , budgets of the total metal content present in galaxy disks, and measurements of chemical abundance patterns that constrain formation timescales. I will discuss ongoing work to reduce systematic uncertainties on metallicity and abundance pattern determinations at high redshift, leading toward a new era of precision chemical abundance studies of the early universe. I will also show new results based on early spectroscopic James Webb Space Telescope data that demonstrate the transformative impact JWST will have on our understanding of galaxy formation at high redshifts.
February 1, Shany Danieli (Princeton University)
Low mass galaxies and their dark matter halos: lessons learned from satellite galaxies and the dynamics of globular clusters
Abstract: The relationship between galaxies and their host dark matter halos, as probed through studies of individual galaxies and statistically, provides a vital test of cosmological models on multiple scales. Being some of the most dark matter-dominated systems discovered to date, low-mass galaxies provide stringent tests of our cold dark matter model, particularly on small scales. However, because they are intrinsically faint and difficult to identify and characterize, studies thus far have primarily relied on the population of dwarf galaxies orbiting the Milky Way. I will present novel observations of low-mass galaxies beyond our local galactic neighborhood, uncovering their significant diverseness and introducing new astrophysical puzzles. I will discuss a new framework for obtaining constraints on the distribution of dark matter in low-mass galaxies, utilizing the photometry of their globular cluster populations and dynamical considerations. I will also present new constraints on the statistical mapping between satellite galaxies and their host dark matter subhalos enabled by the Exploration of Local VolumE Satellites (ELVES) survey, which constructs a unique sample of satellite galaxies beyond the Milky Way. I will conclude by discussing ongoing and future surveys that will be essential in mapping the census and properties of the general population of low-mass galaxies.
February 8, Matt Hosek (UCLA)
Star Formation Near the Galactic Center: New Insights from HST + Gaia
Abstract: The Milky Way Galactic Center provides a unique view for studying how stars form near a supermassive black hole. Young and massive clusters in the region, such as the Arches and Quintuplet clusters, are valuable probes into how star formation is impacted by an environment that is much different than that near our Sun. We combine multi-epoch Hubble Space Telescope (HST) observations with the Gaia satellite catalogs to perform proper-motion based studies of these clusters, identifying cluster members over a much larger area than previously possible and measuring their motion in the rest-frame of the galaxy. I will show how we use these measurements to constrain the past orbits of the clusters, testing different proposed mechanisms for how they formed, and measure their stellar Initial Mass Functions. I will discuss what these clusters teach us about how star formation is triggered near the Galactic Center and how the extreme environment impacts the masses of the stars produced there.
February 15, Steph Sallum (UCI)
Constraining Planet Formation and Evolution with Interferometry and Spectroscopy
Abstract: We have now discovered thousands of exoplanetary systems that inform our understanding of planet formation and evolution. Despite this wealth of data, we still know remarkably little about the details of how forming planets accumulate material, and how the atmospheres and orbital configurations of mature planets evolve over time. Addressing many fundamental questions in this field requires directly characterizing a sample of exoplanets with a variety of ages, masses, and orbits. While we have begun to achieve these observations for a small subset of the exoplanet population, building the census of directly-characterized planets requires improvements in both instrumentation and data processing. I will highlight some of my group’s work in these areas, aimed at pushing the capabilities of direct imaging instruments to expand the exoplanet characterization space. This will include applying high resolution imaging techniques to direct planet formation studies, developing cutting-edge instrumentation for 10-meter-class telescopes, and preparing for enhanced exoplanet science with upcoming observing facilities.
February 22, Enrico Ramirez-Ruiz (UCSC)
Cosmic alchemy in the era of gravitational wave astronomy
Abstract: The source of about half of the heaviest elements in the Universe has been a mystery for a long time. Although the general picture of element formation is well understood, many questions about the astrophysical details remain to be answered. Here I focus on recent advances in our understanding of the origin of the heaviest and rarest elements in the Universe.
March 1, Björn Benneke (University of Montreal)
From hot gas giants to temperate exo-Earths: a new era of exoplanet characterization with JWST and next-generation high-resolution spectrographs
Abstract: We are at the dawn of a new era for planetary astronomy. With our first big JWST results coming out and a new generation of high-resolution spectrographs going into service, our initial results leave little doubt that the upcoming decade present a truly unique opportunity to understand planets and their atmospheres and climates in the most general way. The opportunity is no less than assessing the full diversity of planets in the Universe and finally answering humanity’s millennia-old questions of “Are we alone?” and “How did we get here?”. In this colloquium, I will provide you with a first look into this new era by presenting an overview of our latest results with JWST and ground-based high-resolution spectrographs. My discussion will include the first JWST transmission spectrum of a habitable-zone rocky world outside the solar system, a discussion of the intriguing nature of the long-hypothesized “water-world” exoplanet, as well as the incredible complementary detail JWST and high-resolution spectrographs can provide to probe the formation, evolution, and atmospheric physics of giant planets.
March 8, Kristen McQuinn (Rutgers, The State University of New Jersey)
Galaxy Evolution at the Faint-End of the Luminosity Function, with a Highlight from the JWST ERS Program on Resolved Stars
Abstract: Small galaxies are key tools for understanding structure formation and galaxy evolution. Traditionally defined as galaxies below a mass threshold of ~10^9 Msun, they have long been used to study the individual components of galaxies (stars, gas, chemical elements) and are also used as tests of our cosmological models. We are now finding small galaxies in our Local Group with Mstar as low as 10^3 Msun and gas-rich, star-forming galaxies at slightly farther distances with Mstar ~10^5-10^7 Msun. These extremely low-mass systems approach regimes where theoretical predictions of their physical properties begin to diverge based on different assumptions of their baryonic and dark matter physics and in reionization models. As such, these galaxies can be used to explore questions about galaxy formation, survival, and evolution.
In this talk, I will (i) show recent results characterizing gas-rich, star-forming galaxies to lower masses, with constraints on the changing baryon-to-dark matter ratio in small galaxies, (ii) present the first empirical constraints on the ionizing photon production of a massive O star with a very low metallicity similar to that of early galaxies, and (iii) discuss the newly discovered Local Group galaxy, Pegasus W, which has properties that challenge our models. I will also highlight work from the JWST Early Release Program on resolved stars in three Local Group low-mass systems.
March 15, Santiago Torres (UCLA)
Raining Rocks in Exoworlds: Planet-comets interactions
The dynamical interactions between minor bodies such as comets and asteroids with planets are crucial for understanding the architecture and evolution of planetary systems. These interactions give rise to structures like the Kuiper Belt, the Oort Cloud, and the formation of interstellar comets. In particular, collisions between minor bodies and planets can result in complete planet atmospheric loss and dramatic changes in the orbital architecture of the system. In this talk, I will examine the effects of planet-comet interaction on various planetary system architectures, with a focus on systems detected by Kepler and TESS. Specifically, I will discuss the capture, ejection, and collision of minor bodies with planets and provide new estimates for the endurance of planetary atmospheres under cometary bombardment in different environments.
Fall 2022
October 5, 2022 - Jeff Cooke (Swinburne University of Technology)
The Keck Wide-Field Imager as part of the future direction of the Keck Observatory
Abstract: The Keck Wide-Field Imager (KWFI) is a 1 degree diameter field of view wide-field optical imager for Keck that will be the most powerful wide-field imager in the world or in space for the foreseeable future (decades). KWFI has extreme sensitivity from 10000A down to 3000A that will enable new science from the high redshift Universe, to time-domain science, to the local Universe and the solar system that cannot be done on any other telescope, not even 30m-class telescopes. We have now entered into the era of next-generation facilities, including JWST, 30m-class telescopes, Maunakea Spectroscopic Explorer, NASA Roman space telescope, Cherenkov Telescope Array, Square Kilometre Array, LIGO/Virgo/KAGRA, with larger, more sensitive facilities planned for the next decades, such as the Cosmic Explorer, LISA, LUVOIR, and others. In this talk, I will discuss the need now for KWFI's extremely deep, wide-field imaging and its greater need in the coming decade - as it is vital for nearly all science cases for these facilities (many are billion-dollar facilities) operating at all wavelengths and to greatly extend their reach. I will discuss the status of KWFI, its continued progress, and the development of a deployable secondary mirror to enable new science and fast imaging and spectroscopy capability in the same night.
October 12, No colloquium
October 19, Sera Markoff (University of Amsterdam)
A tale of two black holes: Sgr A* and M87*
Abstract: Black holes are one of the most exotic consequences of Einstein’s General Relativity, yet they are also very common, ranging from stellar remnants up to beasts billions of times more massive than our sun. Despite their reputation as cosmic vacuum cleaners, they actually drive extremely complicated astrophysical systems that can majorly influence their surroundings. Via their powerful outflows in particular, black holes shape the way the Universe looks today...but not at all times. Black holes undergo cycles of activity, so to understand their role over cosmological timescales we need to understand not only how they power these outflows from just outside their event horizons, but also what drives their cyclic behavior. Thanks to the Event Horizon Telescope (EHT) we have now directly imaged the event horizon region for two nearby supermassive black holes: Sgr A* in our own Galactic center, and M87* in the Virgo cluster of galaxies. After a brief review of the key results so far, I will put them into the context of our greater understanding of black hole activity, with emphasis on the gains made by combining EHT observations with those from other multi-wavelength facilities.
October 26, Hilke Schlichting (UCLA)
Rocky Planet Formation with primordial H2-rich Atmospheres: Implications for Super-Earths, Sub-Neptunes and Earth
Abstract: Super-Earths and sub-Neptunes are the most abundant exoplanets discovered to date. Recent models of atmospheric evolution and erosion by core-powered mass loss and/or photoevaporation suggest that these two populations of exoplanets might have been born as one. In these models, close-in, lower-mass planets lose their hydrogen–helium envelopes and become rocky super-Earths, whereas more massive, longer-period planets retain primordial H/He envelopes and remain sub-Neptunes. In my talk, I will explore the question as to how primary, hydrogen-rich atmospheres influence the physical evolution and chemical composition of super-Earths and sub-Neptune exoplanets and as to whether Earth may also have formed from planetary embryos with H2-rich primary atmospheres. Since for most exoplanets, we will only be able to probe atmospheric chemical compositions, understanding their core–mantle–atmosphere connections is likely crucial for correctly inferring the physical properties of their underlaying mantles and cores, which make up the bulk of these planets by mass.
November 2, David Hogg (NYU)
Is machine learning good or bad for astrophysics?
Machine learning is presenting new opportunities for astrophysics—and all the natural sciences. The standard machine-learning workflow represents a very different epistemology and ontology than we're used to in traditional approaches. How does that impact our results and beliefs about those results? I’ll discuss the different roles for machine learning in astrophysics and discuss them in terms of their effects on measurement precision and understanding. I’ll argue that it’s very different to, say, use a Gaussian Process to model stellar variability in a transit measurement than it is to, say, replace an n-body simulation with a deep-learning emulator. I'll also discuss recent work on encoding ideas from classical physics into machine-learning methods.
November 9, Dan Stark (University of Arizona)
Galaxies in the Reionization Era: New Insight from Early JWST Data
Abstract: Deep infrared images from JWST have recently pushed the cosmic frontier back to just 200 million years after the Big Bang, opening a new window on the emergence and growth of galaxies in the redshift range 6 < z < 7. The first images and spectra from JWST are rapidly transforming our understanding of the ages, star formation histories, structure, and metal content of galaxies in the first billion years, revealing a population that is very different from that at later cosmic epochs. In the first part of my talk, I will review my group’s efforts over the last few months to characterize the nature of the earliest star forming sources with JWST. I will describe several of the surprises that have emerged from the early release imaging, while also detailing some of the challenges we face in interpreting existing and upcoming spectroscopic datasets. In the second part of my talk, I will describe the important role that wide area (~7 deg^2) surveys with ALMA and ground-based infrared spectrographs are now playing in advancing our understanding of early galaxy growth, complementing the pencil-beam surveys with JWST. These campaigns are beginning to provide our first glimpse of the progress of reionization around some of the most overdense regions known at z~7, while also revealing new insight into the nature of the first massive galaxies. I will review some of the highlights from these ongoing surveys, while also motivating the potential of upcoming JWST and ALMA observations to build on this progress in the near future.
November 16, Ed Turner (Princeton University)
The Hubble Volume May Well Be Entirely Devoid of Extraterrestrial Life, Intelligence or Technological Civilizations
Abstract: The two most common and apparently compelling arguments for the existence of extraterrestrial life, intelligence and technological civilizations are the (probable) extremely large number of exoplanetary environments similar to the Earth's and the application of the Copernican Principle to abiogenesis, evolution and sociology. On closer examination both of these lines of reasoning are shown to have fundamental flaws. Thus, it remains entirely plausible that the Earth is unique in the observable universe as a home to any or all of these three astrobiological phenomena. The discussion will also illuminate a major unresolved question in our understanding of nature which deserves serious attention independent of the specific topic considered in this presentation.
November 23, Thanksgiving - no talk
November 30, Nahum Arav (Virginia Tech)
The Contribution of Quasar Absorption Outflows to AGN Feedback
Abstract: Central source and their kinetic luminosity are crucial for understanding their contribution to AGN feedback. Here we summarize the results for a sample of nine luminous quasars that were observed with the Hubble Space Telescope. We find that the outflows in more than half of the objects are powerful enough to be the main agents for AGN feedback. The sample is representative of the quasar absorption outflow population as a whole and is unbiased towards specific distance ranges or kinetic luminosity value. Therefore, the analysis results can be extended to the majority of such objects, including broad absorption line quasars (BALQSO).
Spring 2022
March 30, 2022 - Nikole Lewis (Cornell University)
Revealing the Hidden Secrets of Hot Jupiters
Abstract: 51 Pegasi b, the first exoplanet detected around a sun-like star, was the founding member of the hot Jupiter population that now numbers more than 300. Although often derided for their distinct lack of potential habitability and the havoc they likely wreaked in their systems, hot Jupiters have provided a unique opportunity to explore exoplanet atmospheric physics and chemistry. Here I will discuss recent observations of hot Jupiters with the Hubble and now retired Spitzer space-based telescopes that have revealed unexpected processes at work in these distant worlds. I will also discuss current limitations in our ability to interpret observations of hot Jupiters in order to understand the physics and chemistry that shape their atmospheres. Additionally, I will overview observations of hot Jupiters planned for the recently launched JWST and what we hope to learn by exploring these planets with infrared spectroscopy. Although hot Jupiters have been revealed to possess complex atmospheres, they still remain one of our best opportunities to hone observational techniques and atmospheric theories along the path to answering the questions “How did we get here?” and “Are we alone?”
April 6, 2022, 3:30pm - Marc Kamionkowski (Johns Hopkins University)
The Hubble tension and early dark energy
Abstract: The value of the cosmic expansion rate (the Hubble constant) inferred from observations of supernovae disagree with those inferred from measurements of the cosmic microwave background. Easy explanations for this discrepancy have been elusive, but the past few years attention has turned to the possibility that a modification to early-Universe physics may be required. I will discuss a solution to this "Hubble tension" that involves the introduction of a new component of matter, “early dark energy,” as well as other related ideas.
April 13, 2022 - Katherine R. de Kleer, Caltech
The surface environments of the galilean satellites
Abstract: The galilean satellites of Jupiter provide a laboratory for studying geological activity and its role in surface-interior exchange on planet-scale bodies. The differing degrees of tidal heating in these four satellites play out clearly in the level and style of their activity, from the intense volcanism of Io through the elusive plumes of Europa to the remnants of ancient activity on Ganymede. Callisto orbits outside the orbital resonance, presenting a control case of a long-inactive moon. Active internal processes manifest on the surface in the form of heat and materials delivered from the interior, providing specific detectable signatures that act as windows into the interior. High-resolution multi-wavelength telescope datasets from visible and near-IR (HST/Keck) through millimeter (ALMA) wavelengths sense different depths, from the subsurface up through the tenuous exosphere. This talk will discuss how such datasets are helping us understand the surface environments of these objects and the links between their interiors, surfaces, and atmospheres, and will present some outstanding questions that will be addressed by upcoming missions and observatories.
April 20, 2022 - Bruce Macintosh (Stanford)
Direct Imaging of Extrasolar Planets
Abstract: Direct detection of extrasolar planets - spatially resolving a planet from its host star while blocking, moving, or post-processing the starlight - is a powerful complement to transit, RV, and microlensing approaches. Direct detection is sensitive to planets in wider orbit, and allows spectroscopic characterization of planetary atmosheres. One of the most effective instruments in this regime has been the Gemini Planet Imager (GPI). GPI was a facility instrument combining advanced adaptive optics, a diffraction-controlling coronagraph, and an infrared integral field spectrograph on the Gemini South Telescope. From 2014-2019 we carried out the Gemini Planet Imager Exoplanet Survey (GPIES), which observed 532 young (10-200 Myr) nearby stars. I will summarize the key results of the GPIES program, including constraints on giant-planet distributions and atmospheric properties. We have also extensively characterized GPI’s performance, leading to insights into next-generation systems.
With current technology, direct imaging with GPI or other instruments is sensitive primarily to planets that are significantly younger than, more massive than, and in wider orbits than Jupiter, and such planets are rare. Moving beyond this will require new capabilities. The GPI 2.0 project upgrades the existing instrument with faster adaptive optics, better coronagraph designs, and new spectrograph modes.When deployed on Gemini North, GPI 2.0 will be able to search younger stars in the Taurus and Ophiucus star-forming regions, and be sensitive to Jupiter-like “cold start” planets. I will summarize the science drivers that guided the GPI 2.0 upgrade and the project’s status.
In the even longer run, direct imaging is the best path to characterizing true Earth analogs - planets orbiting in the habitable zone of sunlike stars, beyond the reach of practical transit spectroscopy. Such detection will require a dedicated space mission incorporating an advanced coronagraph. The recent Astro2020 Decadal Survey laid out a vision leading such a mission over the next decades. Finally, I will summarize the path forward for direct imaging leading to that possible Earth.
April 27, 2022 - Kartik Sheth (NASA HQ)
IDEA (Inclusion, Diversity, Equity and Accessibility) to Actions
Abstract: Inclusion and diversity are increasingly being recognized as crucial ingredients for innovation and success. But unlike a mathematical equation, converting good intentions to successful actions is significantly harder in these human-centered challenges. In this presentation, I will describe some of my 2+ decades of work in the areas of inclusion, diversity, equity and accessibility and discuss successes and failures of different approaches.
May 4, 2022 - Katerina Chatziioannou (Caltech)
Understanding neutron stars and dense matter with gravitational wave signals
Abstract: Detections of neutron stars in binaries through gravitational waves offer a novel way to probe the properties of extremely dense matter. In this talk I will describe the properties of the signals we have observed, what they have already taught us, and what we expect to learn in the future. I will also discuss how information from gravitational waves can be combined and compared against other astrophysical and terrestrial probes of neutron star matter to unveil the properties of the most dense material objects that we know of.
Winter 2022
1/12/2022 - No colloquium due to the AAS!
1/19/2022 - Anna Quider (Assistant Vice President for Federal Relations - NIU)
Title: The Federal Science Budget and Policy: A Primer for Astronomers
Abstract: The US federal government touches all aspects of our lives through its $6.8 trillion annual budget, laws, regulations, rules, and policies. Physics and astronomy are no exception. Physics and astronomy research is dependent upon financial support from an alphabet soup of federal agencies: DOD, DOE, NASA, NIST, and NSF, for example. Decisions are made from the White House and Congress down to individual program managers that shape what research gets done, how research is done, and who gets to do it. This talk will introduce federal science policy by examining the current federal science funding and policy landscape and exploring its impact on the fields of physics and astronomy.
1/26/2022 - Jack Singal (University of Richmond)
Title: How Bright is the Radio Sky? We Don't Know...yet
Abstract: The actual level of diffuse radio emission on our sky is surprisingly uncertain. Almost all investigations that depend on understanding the radio sky, including cosmic microwave background and 21 cm cosmology foregrounds, ultimately rely on just one measurement - the 408 MHz Haslam map from the 1980s, which traces its absolute calibration to highly uncertain, low resolution blocked aperture measurements from the 1960s and earlier. The question of the absolute level of diffuse radio emission has taken on additional urgency given the claimed high radio synchrotron background level from the ARCADE instrument and other recent measurements. Such a high level of background radio emission would require a new population of incredibly numerous, faint radio sources in the universe, or for our Galaxy to be highly anomalous. This talk will discuss the present situation and the project to make the first ever reliably absolutely calibrated large-scale radio map, using the unique features of the Green Bank Telescope combined with custom instrumentation. This polarization sensitive map of the whole sky North of -47 degrees declination with all Galactic latitudes observed will provide an important new resource for understanding and constraining almost all Galactic and extragalactic phenomena that manifest in, or depend on the understanding of, diffuse radio emission.
2/2/2022 - Wen-fai Fong (NU)
Title: Illuminating the Origins of Fast Radio Bursts
Abstract: When we look up at the night sky, we see a static universe. However, observational surveys have revealed that our universe is dynamic with a myriad of transient events. One of the universe's most fascinating and fastest explosive transients to come to light over the past decade are fast radio bursts. While fast radio bursts are seemingly connected to highly-magnetized neutron stars and are among the most prolific transients to occur in nature, the precise origins of fast radio bursts remain uncertain. In this talk, I will discuss this population of transients and our quest to understand their origins, primarily through observational studies of their local and host galaxy environments. I will describe our ongoing campaigns with large ground-based telescopes and HST to build legacy samples of their environments and extract crucial information on their host stellar populations. I will also discuss upcoming upgrades to fast radio burst experiments which will provide a flood of new, well-localized discoveries in the near future.
2/9/2022 - Danielle Berg (University of Texas at Austin)
Title: Bridging Galaxy Evolution Across Cosmic Time With the CLASSY Survey
Abstract: Rest-frame far-ultraviolet (FUV) spectra are fundamental to our understanding of star-forming galaxies, providing a unique window on massive stellar populations, chemical evolution, feedback processes, and reionization. The launch of JWST and construction of the ELTs will soon usher in a new era, pushing the FUV spectroscopic frontier to z~15-20. The success of these future endeavors hinges on a comprehensive understanding of the massive star populations and interstellar medium (ISM) gas conditions that power the observed FUV spectral features. I will present the COS Legacy Archive Spectroscopic SurveY (CLASSY) Treasury as a powerful and promising solution. CLASSY is a large HST program creating the first high-quality, high-resolution FUV spectral catalog of star-forming galaxies at z~0. The spectra contain a suite of emission and absorption lines that characterize the massive stellar populations that populate metal poor galaxies, the physical properties of large-scale outflows that regulate star formation, and the chemical abundance patterns of the gas and stars. Interestingly, CLASSY is consistent with the z∼0 mass-metallicity relationship, but is offset to higher star-formation rates by roughly 2 dex, similar to z~2 galaxies. This unique set of properties makes the CLASSY atlas the benchmark training set for star-forming galaxies across cosmic time.
2/16/2022 - Maya Fishbach (NU)
Title: Astrophysical Lessons from LIGO-Virgo's Black Holes
Abstract: LIGO and Virgo have observed over 80 gravitational-wave sources to date, including mergers between black holes, neutron stars, and mixed neutron star- black holes. The origin of these merging neutron stars and black holes -- the most extreme objects in our Universe -- remains a mystery, with implications for stars, galaxies and cosmology. I will review the latest LIGO-Virgo discoveries and discuss some recent astrophysical lessons, including mass gaps, evolution with cosmic time, and implications for cosmology. While the latest gravitational-wave observations have answered a number of longstanding questions, they have also unlocked new puzzles. I will conclude by discussing what we can expect to learn from future gravitational-wave and multi-messenger discoveries.
2/23/2022 - Kareem El-Badry (Institute for Theory and Computation in the Harvard/Smithsonian Center for Astrophysics)
Better together: binary stars as probes of star formation and evolution
Abstract: Binary stars are foundational to modern astrophysics. They underpin precision measurements of stellar structure, age, and composition; they provide the most stringent tests of general relativity, they make possible the study of faint and rare objects such as black holes and neutron stars, and they are the progenitors of gravitational wave sources. The components of binaries often interact, dramatically changing their evolution and giving rise to a spectacular zoo of astrophysical phenomenology. To understand stars -- particularly massive stars -- it is necessary to understand binaries. Large-scale stellar surveys such as Gaia, TESS, and SDSS-V are transforming the binary field, making possible both comprehensive population demographics and the discovery of rare objects. I will discuss new insights gleaned from surveys in recent years, including the creation of stripped-envelope stars following binary mass transfer, the formation of equal-mass "twin" binaries in circumbinary disks, and the characterization of planets in binaries. I will focus in particular on the search for dormant stellar-mass black holes in binaries, discussing recent candidates and the path forward to characterizing the detached black hole population.
3/2/2022 - Kirk Barrow (Stanford/SLAC)
High-Cadence Synthetic Observations and Neural Networks in the Era of JWST
Abstract: As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.
3/9/2022 - No colloquium
Virtual Astronomy Colloquia are held via Zoom. Meeting information will be sent in email.
Fall 2021
10/6/2021 - Peter Behroozi (University of Arizona)
Title: Trinity: Unveiling the Connection between Halos, Galaxies, and Supermassive Black Holes
Abstract: We present a new empirical model, Trinity, that observationally constrains the joint relationship between supermassive black holes (SMBHs), galaxies, and dark matter halos from z=0 to z=7. Trinity is unique in its ability to systematically combine constraints from a wide variety of SMBH and galaxy observations, allowing the resulting inferences to be free of theoretical assumptions that have been present in past models. We can hence recover the average growth and merger histories of all detectable SMBHs, describe the evolution of the SMBH—galaxy relationship through time, and even constrain the cosmic evolution of physical SMBH properties such as the radiative efficiency. We also provide a natural solution to the origin of the high accretion rates necessary to grow the largest SMBHs observed at z>6.
10/13/2021 - Sukanya Chakrabarti (RIT)
Title: Towards precision measurements in Galactic dynamics
Abstract: For more than a century now, astronomers have used kinematic analysis, i.e., modeling the positions and velocities of stars, to estimate the accelerations of stars that live within the gravitational potential of the Milky Way. Recent observations have revealed that our Galaxy had a highly dynamic history. For time-dependent potentials (like that of our Galaxy), there are discrepancies between the true acceleration and that derived from kinematic estimates. I will review two independent methods that we have developed to directly measure the accelerations of stars in the Milky Way using extremely precise time-series observations. I will first review our work on measuring accelerations from high precision RV observations conducted over decade-long baselines. In particular, I will discuss theoretical expectations of the vertical acceleration profile that are motivated by Gaia observations. I will then talk about our analysis of pulsar timing observations, from which we were able to measure Galactic accelerations for the first time, and from these measurements, derive fundamental Galactic parameters, including the Oort limit, the local dark matter density, and the oblateness of the Galactic potential. I will end by talking about prospects for measuring dark matter sub-structure with our ongoing ESPRESSO observations, and the possibility for developing an “acceleration ladder”.
10/27/2021 - Chuck Horowitz (Indiana University)
Title: Supernovae Ignited by Nuclear Fission
Abstract: Type 1A supernovae (SN Ia) are giant stellar explosions that provide important distance indicators in cosmology. Presently there is tension between Hubble constant values determined from SN and from other means. SN Ia are thought to involve white dwarf stars, but it is unclear how they explode. We propose a new mechanism involving a natural nuclear fission explosion. White dwarfs cool and eventually crystalize. Our molecular dynamics simulations find that the first solids to form, as the star cools, are greatly enriched in actinides such as uranium. This is because actinides have the highest nuclear charge. These solids may support a fission chain reaction that, in turn, could ignite carbon fusion and explode the star. This physics parallels that in terrestrial nuclear weapons.
11/3/2021 - Claude-Andre Faucher-Giguere (Northwestern University)
Title: Simulating galaxy formation with FIRE: some results on the role of feedback and of the circumgalactic medium
Abstract: Galaxies are remarkably diverse in their properties, ranging from irregular to disky to elliptical in morphology, and from blue to red in color. At the same time, when analyzed systematically, galaxy populations exhibit striking regularities, with clear trends with mass and redshift. How does this "regular complexity" emerge from the hot Big Bang? I will present results from the FIRE simulations which shed some light onto the processes that shape galaxies. The FIRE zoom-in simulations resolve the multiphase interstellar medium of galaxies and model several different feedback processes (including Type II/Ia supernovae, stellar winds, and radiation) while including the cosmological environment. I will highlight predictions for the formation of disk galaxies, the "burstiness" of star formation, and galactic winds. I will also summarize recent results on a phase transition experienced by circumgalactic gas as halos grow (the virialization of the CGM), and discuss how the interplay between feedback on small scales and the physics of halo gas on larger scales may drive important aspects of galaxy evolution.
11/10/2021 - Ruth Angus (American Museum of Natural History)
Title: Measuring the Ages and Rotation Rates of Cool Stars with TESS and Other Photometric Surveys
Abstract: It has been 50 years since the discovery that stellar rotation periods can be used to date stars, however, converting a rotation period to an age via 'gyrochronology' is still far from simple. In fact, each time a new batch of data becomes available, the relationship between stellar rotation period and age is revealed to be even more complex than previously thought. Light curves from the TESS mission provide an opportunity to measure the rotation rates of millions of stars in the Solar neighborhood, which could help to refine gyrochronology models. However, although TESS provides incredible sky-coverage, its light curves are relatively short, just 27 days long, and it proves difficult to measure rotation periods longer than around 14 days for any star with TESS, even those with a year of near-continuous monitoring. Measuring rotation periods with TESS and measuring ages from those rotation periods are both non-trivial tasks, but a catalog of TESS rotation periods and ages would be a rich repository for scientific opportunity. In the near future, the Vera C. Rubin observatory will provide an overwhelming number of light curves for stars across the Galaxy. Can we refine our age-dating and period-measuring techniques in time to fully leverage the incredible data set of LSST? In this talk, I will discuss ongoing efforts to turn photometric survey data into an archive of stellar rotation periods and ages which could reveal the evolutionary history of our Galaxy, its stars, and the planets that orbit them.
11/17/2021 - Vikki Meadows (University of Washington)
Title: Do The Clouds of Venus Contain Phosphine?
Abstract: In late 2020, the observation of a 266.94 GHz feature in the Venus spectrum was attributed to phosphine (PH3) in the Venus clouds, suggesting unexpected geological, chemical or even biological processes. Since then, the planetary science and astronomy communities have engaged in a number of important scientific tests of the Venus PH3 hypothesis. These include re-analyzing the original discovery data, searching for corroborating features elsewhere in the Venus spectrum, and exploring alternative explanations for the detection and interpretation of the 266.94 GHz line. Many of these steps can be considered part of a larger scientific framework for biosignature assessment. In this talk I will review the discovery papers, and describe a comprehensive research effort to independently analyze both the data and the phosphine interpretation for the 266.94 GHz line. Our work suggests an alternative hypothesis—that typical amounts of Venus SO2 can fully explain both the detection and non-detection of absorption lines in the discovery data. This study further emphasizes the importance of understanding planetary context when searching for, and interpreting, potential signs of life beyond the Earth.
11/24/2021 - Thanksgiving (no colloquium)
12/1/2021 - Jamie Law-Smith (UCSC)
Title: Interactions between black holes, stars, and galaxies
Abstract: A physical understanding of the high energy interactions between black holes and stars, coupled with the context of their galactic birthplaces, will allow us to use these systems as tools to better understand black holes at all masses, the lives and deaths of stars, and the dynamical mechanisms operating in galaxies. In this talk, I will discuss one particular interaction: the tidal disruption of a star by a supermassive black hole. I will present a library of tidal disruption event simulations and will show that it can be reduced to a single relationship. I will present the chemical structure of the disks formed after tidal disruption, which is important for understanding the spectra of these events. I will also connect these AU-scale events to kpc-scale galaxy physics: I will present a systematic study of tidal disruption event host galaxies in the context of the local galaxy population, and in particular our finding that they are highly centrally concentrated. We expect ~50,000 tidal disruption events detected with Rubin over 10 years, allowing us to use these events as unprecedented probes of supermassive black hole demographics, nuclear stellar populations, the physics of super-Eddington accretion, and dynamical mechanisms operating in galactic centers.
Summer 2021
Abstract: I will present the most recent results of the deep line surveys of TMC-1 and IRC+10216, performed with the YEBES 40m and IRAM 30m radio telescopes, and with the ALMA interferometer. These surveys cover the frequency ranges 31-50, 70-116, 120-180, and 200-350 GHz. In the case of TMC-1 our data show several hundred U-lines in the 31-50 GHz range that certainly arise from several tens of new species, probably hydrocarbon radicals. For IRC+10216 the ALMA data show a forest of more than 1500 narrow U-lines arising from the dust formation zone for which we have not found any obvious carrier candidate. Although the chemistry of a circumstellar envelope (IRC+10216) could be, a priori, unrelated to that of a protostellar dark core (TMC-1), we have found that the comparative study of their chemical composition can provide key information on the role of ion-neutral and radical-radical reactions. Time plays a critical role in the growth of cyclical molecules in circumstellar envelopes. However, in interstellar clouds radical-radical reactions permit the development of a rich chemistry leading to the formation of pure hydrocarbon rings, including the first non-functionalized PAH, indene (c-C9H8).
Spring 2021
Abstract: Multiple-planet systems composed of close-in super-Earth/sub-Neptune-sized planets are ubiquitous, representing a dominant outcome of planet formation. This population exhibits predictable hallmarks of architectural regularity and uniformity, such as low eccentricities and inclinations, similar orbital spacings, and intra-system correlations in planetary masses and radii. On top of this first-order structure, however, these systems also exhibit surprising anomalies that require explanation. Examples include (1) ultra-short period planets, whose extremely-irradiated orbits have been separated off from the rest of their systems; (2) planets piled up wide of mean-motion resonances; and (3) a subset of Neptune-sized planets that show signs of radius inflation. In this talk, I will propose that tidal dynamics can account for these specific anomalies and more. Specifically, I will discuss the critical role of enhanced tidal dissipation due to non-zero planetary axial tilts (obliquities), which arise by way of prevalent dynamical resonances. I will highlight strategies for testing these tidal theories and observing obliquities directly in the future.
4/7/2021 - Jennifer Burt (JPL)
Abstract: NASA's TESS mission has produced more than 2000 planet candidates to date, and the TESS community is working to achieve the mission's level one science requirement of delivering masses for 50 new TOI planets by Summer 2021. With such a large starting pool, the decision of what candidates to follow up requires the collaboration of numerous ground based facilities. I will discuss the flow down from TESS Object of Interest (TOI) to confirmed planet through the lens of two recent confirmations. The first, TOI-824 b, is a hot, sub-Neptune planet orbiting a K4V star that sits in a crowded section of the night sky. Follow up efforts revealed an incorrect initial TESS radius estimate due to biased background estimates, demonstrating the importance of higher resolution ground based photometric follow up. The second, TOI-1231 b, is a temperate, Neptune-sized planet orbiting a nearby M3V star. Exhibiting only one transit per sector of TESS monitoring, the planet is one of the coolest small planets detected in the primary mission. Models of atmospheric observations suggest that it will be possible to detect spectral features in an atmosphere similar to that of K2-18 b enabling the first comparative planetology in the 250-350 Kelvin temperature range. Both of these new planets offer exciting atmospheric follow up possibilities and move TESS two steps closer to accomplishing its level one science goal.
4/14/2021 - Alan McConnachie (University of Victoria / NRC Herzberg Institute of Astrophysics)
Abstract: It might be a cliché to say that Gaia is revolutionising our understanding of the structure of the Milky Way and its constituent stellar populations, but it is true and cannot be overstated. Most of this revolution is occurring within 10\,kpc from the Sun; beyond this, Gaia parallax uncertainties are of order 100%. However, Gaia proper motions can remain accurate to an interesting level for much more distant objects. We have undertaken an extensive wide field imaging campaign of the northern skies, concentrating on obtaining exquisite u-band data for thousands of square degrees, approximately 3 magnitudes deeper than SDSS. Combined with other bands, these data are excellent for obtaining photometric parallaxes for a wide range of stellar populations. I will show how these data, combined with Gaia proper motions, are allowing for the discovery of new streams and substructures in the very outer parts of the Galaxy (10 – 100,kpc distant), including a feature associated with the globular cluster NGC5466 that promises to be a highly useful galactic potentiometer. I will also discuss how precise proper motions for the entire dwarf galaxy population of the Milky Way (50 – 400kpc distant) are allowing us to examine the association, or otherwise, of groups of globular clusters and dwarf galaxies that point to group accretion events. Finally, I will present new Gaia proper motions for distant, isolated, dwarf galaxies (~500kpc distant), and examine their orbital evolution within the Local Group gravitational potential.
Abstract: The formation of the first galaxies is a most exciting and elusive frontier. A lasting legacy of the Hubble and Spitzer space telescopes is the discovery and characterization of galaxies to redshift z∼11, looking back 97% of the time to the Big Bang. I will review our current sketch of galaxy build-up at cosmic dawn, highlighting fundamental questions that remain unanswered: when did the first galaxies form, what is their role in reionizing cosmic Hydrogen, and how do they evolve into the galaxies we observe at later times? The launch of the James Webb Space Telescope later this year will be an absolute game changer. JWST will deliver ultra-sensitive imaging and spectroscopy at wavelengths previously inaccessible. I will look ahead and discuss several initiatives in Webb's first year that address key outstanding issues, including our program UNCOVER, which aims to explore the so-called "Dark Ages" (10 < z < 20), the period after Recombination when the first stars and galaxies formed.
Abstract: The Observations of Redshift Evolution in Large Scale Environments (ORELSE) Survey is a systematic photometric and spectroscopic search for structure on scales > 10 Mpc around 18 known clusters at 0.6 < z < 1.3. The survey covers 5 square degrees, all targeted at high-density regions, making it comparable in area and spectral coverage to historic extragalactic field surveys. The goal of the survey is to study galaxy evolution across all scales -- from dense cluster cores to infall/intermediate-density regions to the field. In this talk, I describe the survey design, the galaxy sample, and our novel environmental metrics. I present some recent results on using the large galaxy sample to create a quantifiable cluster catalog, measure galaxy properties as a function of stellar mass, environment, and redshift, and constrain the nature of the active galaxy population. Finally, I describe our latest survey C3VO, which combines ORELSE with the higher-redshift survey VUDS to chart cluster formation and its effect on member galaxies over the last 12 billion years.
5/26/2021 - Emily Rice (City University of New York)
Science of All Stripes:
Creating an Eclectic Academic Career and Broadening Inclusivity
The landscape of academic science has changed significantly in recent decades and is poised to change even more in the near future. We can leverage these cultural changes to create an environment that is both inclusive to more people and effective in preparing students (science majors and non-majors alike) for a wider variety of careers and more broadly defined success. I’ll share my own path to science, including graduate school at UCLA, and a variety of science projects I have been involved in along the way to becoming tenured faculty at the City University of New York, including: planetarium shows, parody music videos, media appearances, Astronomy on Tap public outreach events, STARtorialist science fashion blog and shop, the AstroCom NYC research mentorship program, and the BDNYC brown dwarf research group. The implicit mission that connects these eclectic projects is to expand support for, participation in, and even the definition of science.
Winter 2021
Abstract: Sub-Neptune, super-Earth size exoplanets are a new planet class. Though absent from the Solar System, they are found by microlensing, radial velocity, and transit surveys to be common around distant stars. In this talk, I'll review both recent developments and outstanding puzzles in our understanding of the nature and origin of these enigmatic planets.
1/20/2021 - Ilya Mandel (Monash University)
Title: The promise of gravitational-wave astrophysics
Abstract: The first detections of gravitational waves from compact-object mergers have opened up new opportunities and challenges in astrophysics. I will survey the plausible formation scenarios for merging compact-object binaries. I will then describe ongoing efforts to extract the astrophysical evolution of massive stellar binaries from observations of gravitational waves emitted during mergers of the stellar remnants.
1/27/2021 - Charlotte Mason (Harvard/CfA)
Title: Constraining Reionization with Lyman Alpha Emission
Abstract: The reionization of hydrogen in the Universe's first billion years was likely started by photons from the first galaxies. We will probably never observe these galaxies directly, but their properties can be inferred by measuring the timeline and morphology of reionization. I will describe how we can use galaxies at our current observational frontiers to measure the reionization process. In particular, both the strength and line shape of Lyman alpha (Lyα) emission can probe the intergalactic medium (IGM), but modelling physics from pc to Gpc scales is required. I will describe how we can constrain the timeline of reionization and properties of ionizing bubbles by comparing observations of both Lyman-break and Lyman-alpha selected galaxies to models and simulations using statistical inference methods. I will present measurements which favour a late and relatively rapid reionization, and place these in the context of high redshift galaxy formation.
Abstract: The explosion mechanism of Type Ia supernovae (SN Ia) is unknown. The continuity in the properties of SNe Ia across the luminosity function suggests a single dominant channel to explain the population. We argue that direct collisions of white dwarfs may be promising as such a major channel. I will present results of our efforts to test the collision model.
2/10/2021 - Natalie Hinkel (Southwest Research Institute)
3/10/2021 - Brad Hansen and Ben Zuckerman (UCLA)
Title: Fight or Flight? Exploring some options available to long-lived technological civilizations in the Milky Way
Abstract: We will give two 25 min talks related to the astrophysical constraints on the lifetime of a technological civilization in the Milky Way, in the face of stellar evolution of its original host star.
Fall 2020
Abstract: I will present a combination of three observational techniques--astrometry, radial velocity, and imaging--to discover, weigh, and characterize massive exoplanets and brown dwarfs. While thousands of planets are known, only a few have both measured masses (from radial velocity and astrometry) and atmospheric properties (inferred from spectra). Advances in adaptive optics and infrared instrumentation now enable us to see young exoplanets millions of times fainter than their host stars. Despite huge gains in sensitivity, however, high-contrast imaging surveys remain plagued by a lack of discoveries. I have calibrated a huge data set of stellar reflex motions; it can identify unseen planets and brown dwarfs by the gravitational tugs they exert on their host stars, and enable us to measure their masses and orbits. With masses, orbits, and spectra of a growing sample of planets and brown dwarfs, we can finally test models of substellar formation and evolution.
Abstract: Massive galaxies reside in the densest and most evolved regions of the Universe, yet we are only beginning to understand their formation history. Today massive galaxies are red and dead ellipticals with little ongoing star formation or organized rotation; naturally they were expected to be relics of a much earlier formation epoch. In this talk I will describe the complex evolutionary history of massive galaxies that has emerged over the last decade, discussing the structural and kinematic evolution of massive galaxies during and after they stopped forming stars (“quenched”) and eventually transformed from rotationally supported disks into kinematically hot ellipticals. I will describe ongoing efforts to better understand this metamorphosis at intermediate redshifts, highlighting results from the ultra-deep LEGA-C spectroscopic survey of ~3000 massive galaxies at z~0.8 and the focused multi-wavelength SQUIGGLE survey of post-starburst galaxies at z~0.6 caught immediately following their cosmic shutdown. I will show that early quiescent galaxies, retained significant rotational support (~twice as much as local ellipticals), implying that the mechanisms responsible for shutting down star formation do not also have to destroy ordered motion. Furthermore, I will describe first results from the SQUIGGLE survey, including the ALMA discovery of vast reservoirs (~1010 Msun) of cold molecular hydrogen remaining in young post-starburst galaxies caught a few 100 Myrs after quenching their primary episodes of star formation. This enigmatic result suggests that the quenching process does not have to fully heat or deplete the gas to halt star formation. Finally, I will discuss prospects for extending spectroscopic studies of galaxies at cosmic noon - the peak of massive galaxy formation and shutdown - with JWST and eventually 30-m class telescopes.
11/25/2020 - Thanksgiving holiday - no Colloquium