Astrobites at AAS 238: Day 2

Welcome to the virtual summer American Astronomical Society (AAS) meeting! Astrobites is attending the conference as usual, and we will report highlights from each day here. If you’d like to see more timely updates during the day, we encourage you to search the #aas238 hashtag on twitter. We’ll be posting once a day during the meeting, so be sure to visit the site often to catch all the news! 

Image of a face-on grand design spiral galaxy.
This composite image of NGC4535 shows a Hubble image of the galaxy, overlaid with new ALMA observations of the galaxy’s molecular clouds. [ALMA (ESO/NAOJ/NRAO)/PHANGS, S. Dagnello (NRAO)]

LAD Plenary Lecture: Origins of Astrochemical Complexity (by Luna Zagorac)

Astrochemical complexity and its origins is a topic that is just too — well, complex! — to cover in a single plenary. For this reason, Karin Öberg (Harvard University) began with a small amendment to the talk title: she focused on “(Icy) Origins of Astrochemical Complexity (During Planet Formation).” Specifically, she tracked the origins of volatile organic compounds through the process of planet and star formation. In chemistry speak, “volatile” means that these molecules prefer to be in the gas stage, while “organic” means that they necessarily have a carbon (C) atom, often linked to oxygen (O) and nitrogen (N). Understanding where these molecules come from is crucial, because they are the building blocks of life on Earth!

But before we can have life, we have to have a planet. The story of planet formation, roughly, is as follows: first, there is a cloud of dust; as this cloud collapses it forms a protostar in the center, and subsequently a protoplanetary disk around it. This system evolves until it begins to look something like our solar system: a central star with (some terrestrial) planets orbiting it, one of which might contain a life-form. But where along this celestial journey did we pick up enough organic volatile molecules to make up said life-form?

Artist image of the four stages of planetary disk formation connected by dust: a molecular cloud, a proto-star (which kinda looks like a sunny-side-up egg with dust around it), a protoplanetary disk (which looks like just an egg sunny side up), and finally a planetary system (which looks like our solar system).

Image illustrating the stages of planetary system formation. [Bill Saxton, NSF/AUI/NRAO]

The answer: at every stage! First, consider the cloud stage: this is the only stage of the process cold enough (~10 K!) to form ices of volatiles such as methanol, CH3OH. Because these ices are also detected in the later protoplanetary disk, this must mean the ices survive into the next stage of the process! Furthermore, though it’s too cold to spontaneously turn these methane ices into more complicated compounds, lab experiments show that there are a few channels for getting these reactions started. One channel is an influx of energy from a stray cosmic ray, which would break up an icy molecule and send it over its activation potential for reacting with its neighbors; another has to do with oxygen insertion (see Jenny Bergner’s LAD Dissertation Talk Prize for more on this!). Once the protostar forms, it warms up its surroundings to about ~30 K, where not only is it easier to form complex molecules, but different mixtures become possible. All of these compounds are inherited by the protoplanetary disk, which in turn hosts its own in situ chemical reactions further contributing to molecular diversity and complexity.

The takeaway: not only are organic chemical environments of planet-forming regions shaped by cloud, protostellar, and in situ disk chemistry, they are also shaped by ice organic chemistry. For the latter, lab experiments have been and continue to be crucial in identifying new formation pathways and their efficiencies.

Interview of Karin Öberg by Ellis Avallone
Live-tweeting of the session by Luna Zagorac

Press Conference: Molecules in Strange Places (by Tarini Konchady)

The first presentation at this briefing was given by Kate Gold (Bryn Mawr College) and Deborah Schmidt (Franklin & Marshall College). They discussed the preliminary results of a search for molecules around planetary nebulae (PNe). PNe play a key role in determining the chemical content of the interstellar medium, so it’s important to ascertain what molecules can survive the violent irradiation that occurs in the PNe stage. Models suggest that scarcely any molecules make it out intact, but observations point to the opposite being true! Using the 12 Meter Telescope and the Submillimeter Telescope in Arizona, the team searched for signatures of the molecules HCN and HCO+ in 13 PNe of varying ages. Not only did they find significant fractions of these molecules around most of the observed PNe, they also found that the presence of those molecules did not change significantly with PNe age.

A translucent oval cloud sits on a black background with bright white objects. Two broad, even more translucent, orange streams come off the top and bottom of the oval.

A bipolar planetary nebula in the constellation Scutum. [ESA/Hubble & NASA, L. Stanghellini]

The next presentation was given by Lucy Ziurys (University of Arizona) on using ALMA (Atacama Large Millimeter/submillimeter Array) to search for the previously mentioned molecules in other galaxies. Given that PNe are an end stage for some stars, they have a lot to tell us about stellar evolution. One open problem in astrophysics is how we get very non-spherical PNe from roughly spherical stars. With the relatively new discovery that PNe can be molecule-rich, researchers decided to try using ALMA to make “molecular images” of PNe by observing the molecular gas associated with these objects. These images offer a new window into PNe because the cold molecular gas produces features that don’t usually show up in optical images. These results could point us to how PNe are shaped.

The third presentation was given by Lilia Koelemay (University of Arizona) on the detection of organic molecules on the outer edges of the Milky Way. While our galaxy has some assumed habitable zone (the “galactic habitable zone”), organic molecules have been found much further out than the extent of that habitable zone. This motivated another search for organic molecules in molecular clouds at distances between ~42,000 light-years and ~77,000 light-years from the center of our galaxy. The search found that the abundances of the relevant organic molecules didn’t change much with distance — extending the “OZ” or organic zone of the Milky Way. This finding informs our ideas of where life could arise. Press release

A bright orange spiral galaxy on a black background.

An example of a galaxy surveyed in the PHANGS-ALMA survey. The bright orange regions indicate molecular clouds. [ALMA (ESO/NAOJ/NRAO)/PHANGS, S. Dagnello (NRAO)]

The last presentation was given by Annie Hughes (Institut de Recherche en Astrophysique et Planétologie) on the PHANGS-ALMA (PHANGS: Physics at High Angular resolution in Nearby GalaxieS) survey of molecular gas across a large sample of galaxies. Molecular gas is critical to star formation and star formation influences galactic structure, so it follows that we could learn a lot by studying the distribution and properties of molecular gas in a large variety of galaxies. With this in mind, the PHANGS-ALMA survey mapped CO emission across 90 galaxies. With these observations, the team found that molecular clouds in the central regions of galaxies tended to be denser, more massive, and more turbulent than their counterparts on the outskirts. Press release

Live-tweeting of the session by Tarini Konchady
YouTube recording of the session on the AAS Press Office channel

STScl Town Hall (by Sabina Sagynbayeva)

Dr. Nancy Levenson, the deputy director of STScI, reported on the status of the existing and upcoming missions and described new opportunities designed to advance astrophysics through the 2020s.

She started off reporting the most recent status of the institute: Most Institute staff are working from home now. More people will return on-site in the coming months, but STScI will not host visitors or conferences in person through the calendar year due to focus on current missions.

What missions? Here’s a status update on a few:

  • JWST is going to launch later this year!
  • Hubble’s doing great. Cycle 28 is underway, and the review for Cycle 29 will happen this month. STScI encourages you to share your results if you used Hubble or another telescope supported by STScI, and STScI can help disseminate newsworthy findings. Hubble’s program ULLYSES, a large Director’s Discretionary program for the community to obtain a spectroscopic reference sample of young low- and high-mass stars, put out its second data release in March 2021.
  • The Nancy Grace Roman Telescope will provide a Hubble quality with 100 times the field of view. Roman is working toward launch in the mid-2020s. Also, the primary mirror is complete and all WFI science detectors are available. Levenson also reports that ALL data from Roman will be available with zero exclusive access period. Also, Mikulski Archive for Space Telescopes (MAST) can provide data from Hubble, Webb, Roman, Pan-STARRS, and others.

STScI user committees welcome your input! Their reports and contact information are available on the website:

Illustration of a spacecraft in front of the solar system, an exoplanet, a nebula, and distant galaxies.

This artist’s impression of JWST highlights the broad variety of science that has been approved for Cycle 1. [ESA, NASA, S. Beckwith (STScI) and the HUDF Team, Northrop Grumman Aerospace Systems / STScI / ATG medialab]

Next, Christine Chen discussed the JWST Cycle 1 General Observer (GO) Program. Approximately 33.5% of successful proposals are led by PIs from ESA countries, and 4% by PIs from Canada, but overall there were proposals from all over the world. She also reminded us of the Dual Anonymous Review: proposal reviews were conducted with the identities of the proposal teams removed from the proposals, and each panel has a Leveler who helps to keep the panel discussion focused on the selection criteria.

Chen outlined some of the approved proposals:

  • Protoplanetary disks observations will study the chemistry of water and organics in the terrestrial planet forming regions (<5 AU) and use coronagraphic imaging to search for protoplanets in at least 12 disks
  • Transiting exoplanet observations include the study of sub-Neptunes and super-Earths with time-series spectroscopy and planets transiting active M dwarf stars.
  • Nearby Galaxy Observations will contribute to understanding of the stellar populations and ISM within nearby galaxies
  • AGN outflows and feedback observations will leverage 5–28 µm spectroscopy to determine the heating mechanisms for and estimate the energetics of outflows; characterize the molecular gas, dust, AGN, star formation and metallicity within the central regions; and map the AGN’s influence on the distribution of metals and star formation in different environments
  • Galaxy imaging surveys will image the sky using NIRCam (and MIRI), providing the gold-standard imaging data set for galaxy assembly studies, studying the sources responsible for the reionization of hydrogen, and probing the era of the first galaxies, pushing beyond z = 10
  • Galaxy spectroscopic surveys will observe thousands of galaxies using NIRCam and NIRISS WFSS to provide line diagnostics reaching redshifts up to z = 7 and beyond, enabling characterization of the physical properties of galaxies all the way to cosmic dawn

A final point mentioned is that STScI is hosting JWebbinars! These are entirely virtual classes with ~40 participants with hands-on instructions on common data analysis methods for JWST observations. All materials are made available after the classes.

Live-tweeting of the session by Sabina Sagynbayeva

Meeting-in-a-Meeting: Transient Discovery with Machine Learning (by Sabina Sagynbayeva)

Gautham Narayan (University of Illinois at Urbana-Champaign) opened the session with “Deep Learning for Multimessenger Astrophysics.” How can we classify sources in the huge volume of photometric data expected in the future? Narayan presents on the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC), a means of using deep learning to classify the time-domain sky. The primary goal? To set up a massive time-domain simulation infrastructure and jumpstart machine learning photometric classification efforts.

Andrew Vanderburg (University of Wisconsin-Madison) next talked about “Exoplanet Detection using Machine Learning”. The problem in exoplanet detection is that planets are not the only things that cause stars to dim periodically! We have a lot of data from Kepler and TESS, but we need to identify the dimmings that are specifically caused by planets. Machine learning does two things better than humans: it can perform similar tasks much faster, and it can perform pattern recognition, identifying predictive relationships between different observations that are too complex for traditional methods to solve. Vanderburg presented on how these advantages have been leveraged for exoplanet detection with great success, resulting in multiple potential new planets and the first mass measurement of a known planet around an active star.

Michelle Lochner (University of the Western Cape/ South African Radio Astronomy Observatory) next discussed “Transient Classification and Anomaly Detection in the LSST Era.” The Vera Rubin Observatory will produce an incredible dataset, but it is also going to be an incredible challenge. There are rare events that we know exist, e.g. kilonovae, which Lochner calls “known unknowns.” But unknown unknowns are exciting, too! How do we discover new phenomena among 10 million possibilities? An interesting anomaly to one scientist isn’t interesting to another scientist — so here comes active learning. Lochner built Astronomaly, a package for active anomaly detection for astronomical data. By running machine learning algorithms, this pipeline picks up things that are strange and gives an image a score of how “interesting” it is. Lochner concluded by mentioning their mentoring program for women and gender minorities in physics (and they need more mentors!).

Ashish Mahabal (Caltech) talked about “Machine Learning Aided Classification of Transients and Variables in ZTF.” The Zwicky Transient Facility (ZTF) has a catalog of billions of astronomical objects and specialized filters depending on science use cases. It registers hundreds of thousands of events every night. Mahabal provided an overview of parts of the machine learning workflow in place to discover and classify transients by combining ZTF photometry and spectra from the SED Machine (SEDM).

Guillermo Cabrera-Vives (Department of Computer Science, University of Concepción) wrapped up with “Machine Learning within the ALeRCE System: Past, Present and Future”. ALeRCE is an astronomical alert broker — a system that ingests, processes, and redistributes alerts that come from programs like ZTF — or, in the future, LSST. ALeRCE receives an alert stream about possible transient detections, and then applies machine learning to classify the transient, crossmatch it with archival catalogs, and more.

NSF Town Hall (by Macy Huston)

The NSF Town Hall began with updates on Division of Astronomical Sciences (AST) staffing from interim director Chris Smith, followed by updates on observatories and instruments. In recent NOIRLab news, the Dark Energy Survey’s first three years of observations have produced 30 new papers. Meanwhile, the Dark Energy Spectroscopic Instrument (DESI) has completed its trial and begun the five year survey. Exciting news at the Green Bank Observatory is the development of radar capabilities by the NRAO on the Green Bank Telescope.

Finally, the Covid-19 pandemic has caused delays and additional expenses in telescope construction. The Daniel K. Inouye Solar Telescope is now estimated to begin operations at the end of 2021. Its Cycle 1 call for proposals will be May 1, 2022, and the start of steady-state observations is anticipated for November 2022. The Vera C. Rubin Observatory is now estimated to begin operation in the first half of 2024.

Ongoing construction of the Vera C Rubin Telescope. A crane is lifting large machinery into the dome.

The Vera C. Rubin Observatory, pictured under construction in March 2021. [Rubin Observatory/NSF/AURA]

James Neff reviewed the AST division’s programs and budgets. Two new programs for postdoctoral fellows (MPS-Ascend, NSF 21-573) and pre-tenure faculty (MPS-LEAPS, NSF 21-570) have deadlines approaching in mid-June. Funding opportunity deadlines and program leads were reviewed, and are available on their website.

Ashley Vanderley presented the status of the recently collapsed Arecibo Observatory. Cleanup, an environmental assessment, and an investigation of what went wrong are underway. The observatory team also prioritizes historical preservation, salvaging objects such as a receiver and some reflector panels for display at the site or a museum. The Arecibo Observatory Options Workshop is currently underway. Those who did not register in time are able to watch informational talk recordings on the website and submit ideas to [email protected].

The Electromagnetic Spectrum Management (ESM) exists to ensure the scientific community access to portions of the EM spectrum needed for research. This has been expanded from a focus on radio to include infrared and optical concerns, increasing the management team from 1–2 members to 3–4. Their astronomical concerns are keeping clean, wide bandwidths for radio astronomy, keeping dark skies in the optical/IR, and broadening participation.

Lastly, Chris Smith returned to present the NSF’s fiscal year 2022 budget request. The request increased from $8.5B in FY2021 to $10.17B. Their goals prioritize fundamental research, emerging technology, equity, climate science and sustainability, and research infrastructure. They are looking forward to the Astro2020 community recommendations to help guide upcoming year budgets. They will examine science priorities, the required facilities, and how to support a diverse pool of science-engaged people.

Live-tweeting of the session by Macy Huston

Annie Jump Cannon Prize Lecture: Turbulent Beginnings: A Predictive Theory of Star Formation in the Interstellar Medium (by Ellis Avallone)

The first afternoon plenary of AAS 238 Day 2 is by Blakesley Burkhart (Rutgers University), winner of the 2019 Annie Jump Cannon Prize! Dr. Burkhart is an expert in turbulence, a complex phenomenon that affects space at a vast range of scales.

Her talk begins by first highlighting Annie Jump Cannon herself, whose work in the early 20th century set the stage for the now well-established subfield of stellar evolution. Star formation, however, is an astrophysical process that remains largely unsolved. According to Dr. Burkhart, “We really don’t have a good predictive model [for star formation].” Uncertainties in star formation processes, incidentally, reverberate through all aspects of astrophysics, from galaxy dynamics to planet formation.

molecular cloud

How does the interstellar medium collapse to form stars? [NASA/JPL-Caltech/Harvard-Smithsonian]

Next, Dr. Burkhart describes a key question that threads through star formation research: the star formation efficiency problem. If we assume gravity is the only factor that causes gas in the interstellar medium to collapse into stars, we should observe a star formation rate around 250 solar masses per year. However, if we look at our own galaxy, we observe a star formation rate around 3 solar masses per year. This makes one thing abundantly clear: star formation is incredibly inefficient! Our key problem is now focused on not forming stars, i.e., preventing star formation from being too efficient in our models.

Dr. Burkhard notes that when we look at star formation observationally, we find that star formation efficiency rate is around 1% for both close-by and high redshift galaxies. These similarities from such a diverse galaxy sample indicate that there’s something universal about the physics in star-forming clouds. With that, Dr. Burkhart describes the analytical models and simulations that are critical for understanding this problem.

Most analytical models use a lognormal distribution to describe the density of gas in star-forming clouds. This distribution offers a straightforward way to compute properties of a star-forming cloud — like the star formation rate. However, when we look at observations, we find that parameters that we expect to be correlated with one another are not correlated at all. Therefore, the model has to be adjusted! Dr. Burkhart and her group looked to simulations to determine how to adjust the model and found that at high densities, the gas density distribution behaves much more like a power law. They additionally found that the power law distribution agreed much more strongly with observations.

Simulations are also incredibly useful for looking at which physical processes suppress star formation. Dr. Burkhart’s group found that turbulence does not provide support against gravitational collapse in a star-forming cloud, which was quite the surprise! Instead, magnetic fields and feedback from young stars are the processes that prevent the cloud from collapsing efficiently, and therefore do all the heavy lifting against gravity. When they incorporate these factors into their analytical model, they are able to reproduce the star formation efficiency rate and gas depletion time expected in simulations, which bodes well for future comparisons with observations.

Interview of Blakesley Burkhart by Pratik Gandhi
Live-tweeting of the session by Ellis Avallone

Meeting-in-a-Meeting: Measuring the Properties of Stars with Machine Learning (by Mia de los Reyes)

In this session of the “Machine Learning in Astronomy” splinter meeting, we learned about some of the ways data-driven techniques can be used to study stars!

Stella Offner (The University of Texas at Austin) started us off by speaking about “Harnessing Machine Learning to Identify Stellar Feedback.” Stars are messy! They inject energy and momentum into their environments, and this feedback can produce all kinds of features in the interstellar medium. Such features, like bubbles and outflows, are often identified visually — but this is time-consuming, subjective, and hard! Offner described an algorithm that instead uses convolutional neural networks to identify these features. After being trained on simulated maps of molecular emission, this algorithm does a great job of finding structures produced by feedback — it’s even been able to show that the feedback in these features scales almost one-to-one with the number of individual young stars in a molecular cloud!

Next, Anna-Christina Eilers (MIT) discussed “Mapping the Milky Way with data-driven models.” We live in an era of abundant information about the positions, motions, and spectra of stars in the Milky Way, which can be used to answer open questions about our galaxy’s formation and evolution. But these data have uncertainties! Eilers is using machine learning techniques to derive precise distances and to calibrate stellar abundances. For example, by assuming that red giant branch stars have “standardizable” luminosities, Eilers can use photometric and spectroscopic data to predict their distances with high precision. Similarly, stellar abundances can be predicted using a function of stellar properties. These can be used to make precise maps of stellar velocities and abundances in the Milky Way.

Melissa Ness (Columbia University) went more in-depth on stellar abundances with a talk on “Measuring the properties of stars with data-driven computational approaches.” Surveys like APOGEE and LAMOST are providing us with millions of stellar spectra. What information is contained in these spectra, and how can we use them for science? Ness describes how pipelines like The Cannon are able to reproduce stellar spectra with a simple model that includes only a few stellar properties, like effective temperature, surface gravity, and iron abundance. Interestingly, although spectra contain information about many elements, just a few elements (like iron and magnesium) are needed to predict the abundances of other elements. Finally, data-driven techniques can be used to identify stars with outlier spectra, which can help probe the physics of stellar evolution.

Lily Zhao (Yale University) also discussed stellar spectra, but focused more on measuring radial velocities rather than abundances. In the talk “Machine Learning for Extreme Precision Radial Velocity,” Zhao explained that in order to discover an Earth-like planet using radial velocities, we’d need a spectrograph with around 10 cm/s precision. Next-generation spectrographs can reach sub-m/s precision, but spectroscopic effects from stellar activity become a significant source of error. This is where machine learning comes in! Data-driven techniques can effectively reduce the impact of stellar activity on radial velocity measurements.

stellar oscillations

Asteroseismology uses different oscillation modes of a star to probe its internal structure and properties. [Tosaka]

Last but not least, J. Ted Mackereth (CITA / Dunlap Institute / University of Toronto) spoke about “The Stellar Age Revolution, feat. Asteroseismology, Spectroscopy, and Machine Learning.” One of the most precise ways to measure stellar ages is by using asteroseismology, which is classically done by measuring the global properties of stellar oscillations. We can do even better if we use more detailed information about individual frequencies, or if we use additional information from spectroscopy! Again, data-driven techniques can help with this. For example, using combined data from APOGEE abundances and Kepler asteroseismic data, a neural network can significantly improve upon uncertainties in stellar ages. With these more precise measurements, we can start to pick out patterns of ages, dynamics, and abundances in the Milky Way.

LAD Laboratory Astrophysics Prize: Tales from a Life in Laboratory and Observational Molecular Astrophysics (by Luna Zagorac)

The winner of the AAS LAD Laboratory Astrophysics Prize, Geoffrey Blake (Caltech), looked back on a long career of astrochemical achievements in his talk. The Blake group at Caltech focuses on spectroscopy, spanning the range from microwave to infrared and near-optical frequencies. This is equivalent to a range in temperatures from a few to a few thousand Kelvin, allowing them to probe a wide variety of molecular motions in the sky. Blake emphasized the exquisite quality of ALMA data for astrochemistry, noting that his group worked on laboratory instrumentation to bring it in step with the quality and quantity of observational data. On the other hand, the opposite is true when studying chiral molecules with three dipole moments: they are very-well understood in the lab, but they would require circularly polarized light sources in the sky imaged with an instrument at least the size of the Square Kilometre Array to study observationally. Finally, he highlighted how Spitzer data allows us to study ices and gases (including water!) in planetary formation contexts. He closed out his talk with acknowledgements of both his mentors and past and current students and postdocs, noting particularly how lucky he was to become a Duke Microwaver during his time at Duke University, which ultimately led him to discovering his own astrochemical path.

Live-tweeting of the session by Luna Zagorac

LAD Dissertation Prize: Oxygen Insertion Chemistry: A Low-temperature Channel to Organic Molecule Production (by Luna Zagorac)

The graduate thesis written by Jenny Bergner (University of Chicago) was instrumental in the discovery of a new pathway for complex molecules to form in the icy interstellar medium (ISM): it’s no wonder that she won the LAD Dissertation Prize! Recreating the conditions of the ISM in the lab (a temperature of about 10 K and pressure many orders of magnitude below atmospheric), Bergner was able to use infrared spectroscopy to monitor what happened to icy molecules under these conditions. Turns out, an oxygen singlet state (a form of oxygen atom denoted as O(1D)) is able to insert itself directly into the bond between a carbon and hydrogen atom, forming new organic compounds in a process called O-insertion. The kicker? It’s able to do this without any energy input — meaning, it could even happen in the harsh conditions of the ISM!

This process leads to fragmentation, meaning that new but less complex molecules are produced. However, this is true of so-called saturated hydrocarbons, with a single bond between the C and H atom. In unsaturated hydrocarbons, which might have double or triple bonds between two carbon atoms, an analogous process called O-addition can take place, again with no energy input. Thus, O-insertion and O-addition are able to account for much of the astrochemical complexity seen in ISM ice. Furthermore, no other mechanism can explain the production of ethylene oxide (which has been detected in the ISM). Finally, Berger talked briefly about the role of comets in transferring ISM ices into protoplanetary systems. Small grains could not survive this journey, but larger ones were found to experience virtually no loss on this journey.

Interview of Jenny Bergner by Luna Zagorac
Live-tweeting of the session by Luna Zagorac

SPD Harvey Prize Lecture: A Journey from Quiet Sun Magnetic Fields to Flares (by Sabina Sagynbayeva)

The SPD/AAS early career Karen Harvey Prize is awarded in recognition of a significant contribution to the study of the Sun early in a person’s professional career. This year’s winner, Lucia Kleint (University of Geneva), got into research on solar flares accidentally, but she continues to investigate their inner workings today while also trying to understand how to improve solar observations! 

photograph of a stream of material looping off of the sun's surface

What types of stars are most likely to host stellar flares like this one, emitted by our own star and imaged by the Solar Dynamics Observatory? [NASA/GSFC/SDO]

Solar flares are powered by strong magnetic fields; an incredibly useful tool for studying these magnetic fields is polarimetry, a method where polarization of spectral lines are used to reconstruct solar magnetic fields. Dr. Kleint’s PhD focused on the variation of the turbulent magnetic field over the course of a solar cycle. However, they found that polarization gets canceled out due to the sum between positive polarity and negative polarity. But at the Sun’s limb, the polarization is not zero. That’s why they position the spectrograph very close to the limb (5’’ from the limb). In simulations, they can see that the polarization is decreasing. The Hanle effect (depolarization depending on the magnetic field) can help to detect even small magnetic fields. They measured the magnetic field every month and found no variation, a surprising constant from 2007–2010!

Why does the turbulent magnetic field depend so much on the spectral line it’s observed with? Maybe these spectral lines show different things! We need separate images of the Hanle effect, but so far it’s not possible. They are still unable to properly resolve small-scale magnetic fields due to a lack of photons. Here is where DKIST comes in: this behemoth of a solar telescope is able to look at fine scales on the solar surface using multiple spectral lines.

Dr. Kleint continues to look at solar flares today. People have a general idea how solar flares work, but we still have a hard time predicting them. Dr. Kleint is particularly interested in how to predict solar flares, understanding how their energy is dissipated and the evolution of their magnetic structure, and why other sun-like stars produce much stronger flares than what we observe on the Sun.

When solar flares were first observed, interpreting these observations was extremely difficult.  Today, dedicated flare campaigns at numerous observatories around the world have yielded an overabundance of data. One such flare campaign at the Dunn Solar Telescope has observed what NASA has called the best-observed flare, which sparked the authorship of dozens of papers analyzing this single event!

Even with this abundance of flare observations, puzzling things kept showing up in the observations. Observations from the Solar Dynamics Observatory HMI instrument prompted the adoption of a new flare mode. However, the difference in activity between the solar surface and atmosphere at the flare site leaves more questions unanswered. So the question is: Are our models valid for all flares, or only for particular flares? Machine learning has been critical for digging through the mountains of flare observations, however Dr. Kleint wants to know how we can improve instrumentation to address these unanswered questions. 

Photograph of a tall vertical tower with a dome on top, standing alone in a grassy landscape.

Solar Telescope GREGOR at the Teide Observatory, Tenerife, Canary Islands. [H. Raab

Her wish list:

  • So far, we have no regular high-resolution chromospheric magnetic field measurements. Do we need DKIST, or a spacecraft?
  • Advances in flare modeling and analysis (Radyn, RH, STIC, machine learning)
  • Automatic analysis of millions of spectra/images, which may enable flare prediction

The observations wouldn’t be possible without telescopes! Dr. Kleint discussed the recent redesign of the GREGOR solar telescope, located in Spain. The improvements included a new mirror, producing higher contrast; a new optics design, which solved image aberrations; and reduction of vibrations and temperature variations.

There are still many open questions from quiet Sun magnetic fields to flares that are waiting to be explored.

Live-tweeting of the session by Sabina Sagynbayeva

Seminar for Science Writers: Get Ready for Webb! (by Tarini Konchady)

Christine Pulliam and Hannah Braun (Space Telescope Science Institute) introduced this seminar, which is intended to give an overview of the James Webb Space Telescope (JWST) and the science it will do. First, Eric Smith (NASA Headquarters) provided a description of the final months before JWST’s expected launch and the commissioning that will follow. The telescope continues to be tested to ensure it will work after launch, and the Cycle 1 observing programs have been announced (see the summary of the STScI town hall). Following launch, JWST will see a roughly 180-day commissioning, during which it will ready itself to observe. This process includes the deployment of the telescope mirrors and the calibration of the scientific instruments on board. Cooling is also a critical part of this process, since JWST will be observing in the infrared.

JWST sits fully deployed on a dark background speckled with dim white objects. There is a yellow star in the upper left corner beaming light at JWST. The light from the star hits the primary mirror, then the secondary mirror, and is directed into the Integrated Science Instrument Module at the center of the primary mirror.

The path of light along JWST’s mirrors as it is directed towards the scientific instruments. [STScI]

The following speakers focused on the science that will be done by JWST. Dan Coe (Space Telescope Science Institute) discussed how the telescope will allow us to view the oldest galaxies yet — in fact, it will put us in reach of the first galaxies to have formed in the universe. This part of JWST’s mission will include observing the Hubble Ultra Deep Field. One interesting note is that the faintest galaxies JWST will be able to see can be observed in two ways: by staring into seemingly empty patches of sky for a very long time, or by identifying lensing systems. Spectra of these distant galaxies will also be extremely valuable, as they can tell us about the composition of those galaxies.

Next, Ilse Cleeves (University of Virginia) discussed JWST’s potential impact on the study of planet and star formation. Specifically, astronomers are very interested in how formation happens and the chemical composition of the resulting stars and planets. Right now, ALMA has been our best probe of star and planet formation, and its high quality observations have opened many avenues for JWST to explore. These avenues include observing the earliest stages of star formation, characterizing the composition of cold interstellar medium, and constraining the sort of material that forms terrestrial planets.

Two bright identical stars with diffraction spikes sit on a black background. The star on the left is slightly bigger than the star on the right.

Alpha Centauri A (left) and B (right) as seen by the Hubble Space Telescope. JWST will search for exoplanets around Alpha Centauri A. [ESA/NASA]

Knicole Colón (NASA Goddard Space Flight Center) followed with an overview of the exoplanet science that can be done with JWST. Aside from the previously mentioned formation questions, JWST will also be able to study the compositions of exoplanets and their atmospheres. The telescope’s strength here lies in its infrared capabilities; direct imaging of exoplanets will be more viable than it has been before, and a wider range of chemical signatures will be detectable in transiting exoplanets’ atmospheres. JWST will also afford us detailed study into the disks that form planetary systems.

Finally, Heidi Hammel (Associated Universities for Research in Astronomy) covered the solar system science planned with JWST. Given JWST’s observing position, it will not be able to observe much interior to the Earth’s orbit. However, that still leaves a lot to explore! JWST will be able to create surface maps of Mars, tracing dust, water, and other material. It will also be able to explore the diversity in asteroids and comets. The gas giant planets also have a lot to reveal, from why Jupiter’s Red Spot is red to the weather on Uranus. Planetary moons that appear to have water, like Europa and Enceladus, will also be studied. The even more distant Kuiper belt objects will be within JWST’s reach, and the telescope is also ready for unexpected events like the 1994 Jupiter impact.

More information can be found at and

Live-tweeting of the session by Macy Huston
YouTube recording of the session on the AAS Press Office channel

Plenary Lecture: Our Galaxy in Context: Satellite Galaxies around the Milky Way and Its Siblings (by Mia de los Reyes)

Marla Geha (Yale University) wrapped up Day 2 of #AAS238 by discussing the “nieces, nephews, and niblings” of the Milky Way: the low-mass satellite galaxies around Milky Way-like galaxies! Why focus on these small galaxies? The ~60 known satellite galaxies around the Milky Way are useful laboratories for testing theories about cosmology and galaxy formation.

Screenshot of slide titled "Our Galaxy in Context: Satellite Galaxies Around the Milky Way and its Siblings." Logos in the top left corner include the NSF logo and the Howard Hughes Medical Institute logo. Inset in top right shows the speaker's Zoom camera. A large image takes up most of the slide, showing 144 thumbnail images of low-mass satellite galaxies (they mostly look like blurry blue blobs). Image credit in the bottom left corner reads "SAGA Survey satellite galaxies," and text at the bottom of the slide reads "Marla Geha (Yale)."

The title screen from Marla Geha’s plenary talk, showing many of the satellite galaxies identified by the SAGA survey.

From a cosmological standpoint, these galaxies can help us probe the nature of dark matter! One extreme example: “cold” (i.e., non-relativistic) dark matter simulations predict lots of low-mass galaxies (galaxies with stellar masses < 106 solar masses), while “warm” dark matter models predict far fewer of them. Satellite galaxies can also answer questions about galaxy formation and evolution — in particular, what processes turn off (“quench”) star formation in galaxies? Nearly all of the satellites close to the Milky Way have been quenched, while low-mass galaxies further away still have gas and are still able to form stars. Is this “quenching fraction” characteristic of all galaxies that are satellites of more massive galaxies, or is the environment around our Milky Way somehow unique?

In order to make quantitative comparisons between satellite galaxy populations, we need to observe approximately 100 Milky Way-like galaxies. This is where the Satellites Around Galactic Analogs (SAGA) survey comes in! The SAGA survey has so far identified around 40 Milky Way-like galaxies, and many of their satellites look very similar to the Milky Way’s satellites. Overall, the numbers and luminosities of satellite galaxies around Milky Way-like hosts are consistent with what we see in the Milky Way, and with predictions from simulations. But the quenched fractions of satellite galaxies seem much lower than we expect from our galaxy and from simulations! Hopefully more data will help us figure out what’s going on — and maybe soon we’ll be able to study more low-mass galaxies in general, not just ones around Milky Way-like galaxies!

Interview of Marla Geha by Mia de los Reyes
Live-tweeting of the session by Mia de los Reyes

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