Monday, May 20, 2024

High School Student Creates Soundscape of Exploding Stars


Vanya Agrawal creates her sonification with a computer and MIDI board.

More Videos





Using data from the Zwicky Transient Facility, Southern California high school student Vanya Agrawal creates new "space music."

In September 2023, Vanya Agrawal, a senior at Palos Verdes High School, was searching for a science research project. "I've been interested in music since I was very young, and, over the past few years, I've also become interested in physics and astronomy," Agrawal says. "I was planning on pursuing both as separate disciplines, but then I began to wonder if there might be a way to combine the two."

Enter data sonification. Just as researchers design graphs or diagrams or scatterplots to create a visual mapping of their data, they may also develop an audiomapping of their data by rendering it as sound. Instead of drawing a dot (or any other visual symbol) to correspond to a point of data, they record a tone.

Granted, this is highly unusual in scientific research, but it has been done. Her curiosity piqued, Agrawal soon found examples of these sonifications. For example, in 1994, an auditory researcher, Gregory Kramer, sonified a geoseismic dataset, resulting in detections of instrument error, while in 2014 the CEO and co-founder of Auralab Technologies, Robert Alexander, rendered a spectral dataset into sound and found that participants could consistently identify wave patterns simply by listening.

Do these scientific sonifications make you want to sit yourself down in a concert hall to be swept away by the music they create? Well, when you see a scatterplot of supernovae in an astrophysics journal, do you think, "What is that doing in an academic journal? It belongs on the wall of a museum!" Probably not often.

Here is where the artistic effort comes in: representing scientific information in ways that delight the eye or the ear. This was Agrawal's goal, using an astrophysical dataset to make music that could draw in nonscientific audiences and help them to engage with new discoveries about the universe.

Agrawal first approached Professor of Astronomy Mansi Kasliwal (PhD '11), a family friend, to see about finding an appropriate dataset to sonify. She was quickly put in touch with Christoffer Fremling, a staff scientist working with the Zwicky Transient Facility (ZTF) team. Using a wide-field-of-view camera on the Samuel Oschin Telescope at Caltech's Palomar Observatory, ZTF scans the entire sky visible from the Northern Hemisphere every two days, weather permitting, observing dynamic events in space.

Many of the dynamic events observed by ZTF are supernovae, the explosions of dying stars. In the dataset Agrawal received from Fremling of supernova observations from March 2018 to September 2023, there were more than 8,000 of these. She decided that each supernova detection would be one note in the music she was composing.

"I knew the things that I could modify about the music were when the note occurred, its duration, its pitch, its volume, and the instrument that played the note," Agrawal says. "Then it was a matter of looking at the parameters measured in the dataset of supernova observations and deciding which were most significant and how they should be matched up to musical features."

With Fremling's input, Agrawal decided that the five measurements associated with supernova observations that she would sonify would be discovery date, luminosity, redshift (a quantifiable change in the wavelength of light indicating the light source's distance from us), duration of explosion, and supernova type.

"Discovery date of a supernova has an obvious correlation with the time in which its associated note appears in the music," Agrawal says, "and matching the duration of a supernova with the duration of the note and the type of supernova with the type of instrument playing the note also made the most sense." As for the remaining parameters, Agrawal "flip-flopped back and forth with redshift and luminosity, which would go with pitch or volume. But I ultimately decided on having the luminosity correlate to volume because you can think of volume as the auditory equivalent to brightness. If something emits a dim light, that's like a quiet sound, but if it emits a bright light, that correlates to a loud sound. That left redshift to be translated into pitch."

Once parameters had been translated, the pitch values were modified to enhance the sound. Redshift had to be condensed into a tight range of pitches such that the result would be in the most audible range for human ears.

The initial result, according to Agrawal, was less than euphonius. Fremling, who had tried his own hand at setting down sounds in relationship to each supernova, had the same result: The music, he said, "did not sound good at all."

"I don't think I realized how many notes 8,000 actually is," Agrawal says. "I was definitely picturing it to be a lot slower and more spread out, but after converting the data to sound I heard how densely packed the notes were."

To achieve a sparser texture, Agrawal slowed the tempo of the sound file, extending its length to about 30 minutes, and then set about manipulating and enhancing the musicality of the piece. To ensure that the music would evoke outer space, Agrawal rounded pitches to fit into what is known as the Lydian augmented mode, a scale that begins with whole tones which, Agrawal says, "feel less settled and rooted than ordinary major or minor scales. This resembles the scales in sci-fi music, so I thought it would be beneficial for representing the vastness of space." Agrawal then added a percussion track, a chord track that harmonized dominant pitches in the dataset, and effects such as the sound of wind and distorted chattering.

"There is an element of subjectivity in this," Agrawal says, "because, of course, the music isn't what space actually sounds like, even before I began adding musical tracks. It's my interaction with the universe, my interpretation of it through sound. I would find it interesting to hear how other people sonify the same data, how they interact with the same universe."

Agrawal's composition has already been published on the ZTF website, along with a short video of supernova discoveries that uses portions of Agrawal's composition for background music. But Agrawal's imagination reaches well beyond her first composition: "Obviously the parameters will be different for every dataset, but this type of sonification can be done with any dataset. And with the right algorithms, sonifications can be created automatically and in real time. These compositions could be published on streaming services or played within planetariums, helping astrophysics discoveries to reach wider audiences."

Until those algorithms come along, Fremling, Agrawal, and the outreach coordinator of ZTF have created the resources and tutorials needed to enable anyone to sonify ZTF datasets. The aim is to build a library of sonifications that can be offered to educators, artists, science engagement centers, astronomy visualization professionals, and more to improve and enrich accessibility to science. All resources are available.

Of course, new data will come along to shift our perspective on supernovae, and as a consequence, musical compositions featuring them will change too. "Just within the last year or two we have found a new type of supernova, even though people have been studying supernovae since the 1940s and 1950s," Fremling says. Agrawal will need to introduce another instrument into her orchestra. Also, supernova data can be interpreted in different ways. For example, Fremling notes, "some types of supernovae are inherently always very similar in absolute luminosity. The only reason their luminosity varies in the dataset—which Agrawal has translated into volume in her composition—is because these supernovae are occurring at different distances from our observatory at Palomar."

Agrawal is bound for Washington University in St. Louis in fall 2024, planning to double major in music and astrophysics.

Try your own hand at sonifying supernovae!

Written by Cynthia Eller

Source: Caltech/News



Contact:

Cynthia Eller

celler@caltech.edu


Sunday, May 19, 2024

A Giant Cosmic Butterfly's Nature is Revealed

Pan-STARRS and SMA image: The center of this composite image shows IRAS 23077, likely the largest planet-forming disk ever seen, which looks like a giant cosmic butterfly. Data from the Submillimeter Array (SMA) at radio wavelengths is shown in pink, and data from Pan-STARRS at optical wavelengths is shown as a color image. Most of the nearby stars appear as white or red. The star in the center of IRAS 23077 is not visible because its light is blocked by the surrounding disk, which is viewed from the side. The blue PanSTARRS data for IRAS 23077 shows the smallest dust grains, with sizes of only a few micrometers. These dust grains are elevated into the uppermost layers of IRAS 23077's disk and appear as two bright lobes, similar in shape to the wings of a butterfly. The two faint filaments in IRAS 23077's northern region could be remnants from IRAS 23077's formation. The pink SMA data shows larger dust grains, with sizes of about one millimeter. These larger dust grains are coincident with the midplane of the planet-forming disk, where dust grains settle and grow to larger sizes and eventually form planets. Credit: Radio: SAO/ASIAA/SMA/K. Monsch et al; Optical: Pan-STARRS.  High Resolution Image

Labeled Pan-STARRS and SMA image with SMA image inset: The inset for this image shows compelling evidence that IRAS 23077 contains a planet-forming disk. Along with dust grains, the SMA can also observe the cold carbon monoxide gas that comprises the bulk of a planet-forming disk. By measuring its velocity structure and dividing this into "blue-shifted" and "red-shifted" components, showing material moving towards us and away from us respectively, the team showed that the gas is rotating around the central star, as expected for a planet-forming disk. The line in the bottom left shows the diameter of the disk, equivalent to 660 times the distance between the Sun and Jupiter. Credit: SAO/ASIAA/SMA/K. Monsch et al; Optical: Pan-STARRS. High Resolution Image



CfA astronomers using the Submillimeter Array have determined the true nature of a "giant butterfly" in space, providing information about the environments where planets form.

Cambridge, MA--Astronomers have found what is likely the largest planet-forming disk ever seen, which appears like a giant, cosmic butterfly in the night sky. This discovery offers new insight into the environments where planets form.

Officially known as IRAS 23077+6707 (IRAS 23077, for short), this giant cosmic butterfly is about 1000 light-years from Earth and was initially discovered in 2016 by Ciprian T. Berghea from the US Naval Observatory using the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS). However, for years it remained uncharacterized.

Two new papers have now revealed the true nature of IRAS 23077. One paper, led by Berghea and accepted for publication in The Astrophysical Journal Letters, reports the discovery that IRAS 23077 is a young star located in the middle of what looked like an enormous planet-forming disk. In the second paper, published yesterday in The Astrophysical Journal Letters, researchers confirm the discovery of a large planet-forming disk, using the Submillimeter Array (SMA).

The SMA is an array of telescopes in Hawaii jointly operated by the Smithsonian Astrophysical Observatory (SAO) at the Center for Astrophysics | Harvard & Smithsonian (CfA) and the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) in Taiwan. It detects light at millimeter wavelengths, a type of radio wave.

"After finding out about this possible planet-forming disk from Pan-STARRS data, we were keen to observe it with the SMA, which allowed us to understand its physical nature," explains Kristina Monsch, an SAO astrophysicist and a postdoctoral fellow at the CfA, who led the SMA campaign. "What we found was incredible – evidence that this was the largest planet-forming disk ever discovered. It is extremely rich in dust and gas, which we know are the building blocks of planets."

Planet-forming disks - called "protoplanetary disks" by astronomers - are planetary nurseries in which rocky planets like Earth and Mars, and giant planets like Jupiter and Saturn form around young stars. They are rich in dust and gas, and rotate with a specific signature that astronomers can use to infer their sizes, and the masses of their central stars.

Some planet-forming disks are 'edge–on,' meaning they are oriented such that their own dust and gas–rich disks entirely obscure the light emitted from their parent star, as is the case with IRAS 23077. While their stars may be shrouded, the dust and gas signatures of their surrounding disks can still be bright at millimeter wavelengths, as obtained by the SMA.

"The data from the SMA offer us the smoking–gun evidence that this is a disk, and coupled with the estimate of the system’s distance, that it is rotating around a star likely two to four times more massive than our own Sun," said Monsch. "From the SMA data we can also weigh the dust and gas in this planetary nursery, which we found has enough material to form many giant planets – and out to distances over 300 times further out than the distance between the Sun and Jupiter!."

"The discovery of a structure as extended and bright as IRAS 23077 poses some important questions," said co-author Joshua Bennett Lovell, an SAO astrophysicist and an SMA Fellow at CfA. "Just how many more of these objects have we missed? Further study of IRAS 23077 is warranted to investigate the possible routes to form planets in these extreme young environments, and how these might compare to exoplanet populations observed around distant stars more massive than our Sun."

"In addition to gaining brand new data on IRAS 23077, we must also continue the hunt for other similar objects if we are to unlock the story of how extrasolar planetary systems develop in their earliest years," said co-author Jeremy Drake, Astrophysics Chief Scientist at Lockheed Martin's Advanced Technology Center.

IRAS 23077 was initially termed "Dracula's Chivito" by Ciprian Berghea, who grew up in the Transylvania region in Romania, close to where Vlad Dracula lived. In analogy to the famous object “Gomez’s Hamburger”, which is another enormous planet-forming disk that is seen edge-on, they followed the suggestion of Ana Mosquera, Berghea's co-author, to name it after her country's national dish the "chivito," a hamburger-like sandwich from Uruguay.

Besides Kristina Monsch, Joshua Lovell, Jeremy Drake, and Ciprian Berghea, the authors of the ApJL paper are Gordian Edenhofer from the Max Planck Institute for Astrophysics, David J. Wilner, Garrett K. Keating, and Sean M. Andrews from CfA, and Ammar Bayyari from the University of Hawaii.




About the Center for Astrophysics | Harvard & Smithsonian

The Center for Astrophysics | Harvard & Smithsonian is a collaboration between Harvard and the Smithsonian designed to ask—and ultimately answer—humanity's greatest unresolved questions about the nature of the universe. The Center for Astrophysics is headquartered in Cambridge, MA, with research facilities across the U.S. and around the world.




Media Contact:

Peter Edmonds
Interim CfA Public Affairs Officer
Center for Astrophysics | Harvard & Smithsonian
+1 617-571-7279

pedmonds@cfa.harvard.edu


Saturday, May 18, 2024

NASA Images Help Explain Eating Habits of Massive Black Hole

This image of the Andromeda galaxy uses data from NASA’s retired Spitzer Space Telescope. Multiple wavelengths are shown, revealing stars, dust, and areas of star formation.

Data from NASA's retired Spitzer Space Telescope has given scientists new insights into why some supermassive black holes shine differently than others.

In images from NASA's retired Spitzer Space Telescope, streams of dust thousands of light-years long flow toward the supermassive black hole at the heart of the Andromeda galaxy. It turns out these streams can help explain how black holes billions of times the mass of our Sun satiate their big appetites but remain "quiet" eaters.

As supermassive black holes gobble up gas and dust, the material gets heated up just before it falls in, creating incredible light shows — sometimes brighter than an entire galaxy full of stars. When the material is consumed in clumps of different sizes, the brightness of the black hole fluctuates.

But the black holes at the center of the Milky Way (Earth's home galaxy) and Andromeda (one of our nearest galactic neighbors) are among the quietest eaters in the universe. What little light they emit does not vary significantly in brightness, suggesting they are consuming a small but steady flow of food, rather than large clumps. The streams approach the black hole little by little, and in a spiral, similar to the way the water swirls down a drain.

Hunting for Andromeda's Food Source

A study published earlier this year took the hypothesis that a quiet supermassive black hole feeds on a steady stream of gas and applied it to the Andromeda galaxy. Using computer models, the authors simulated how gas and dust in proximity to Andromeda's supermassive black hole might behave over time. The simulation demonstrated that a small disk of hot gas could form close to the supermassive black hole and feed it continuously. The disk could be replenished and maintained by numerous streams of gas and dust.

But the researchers also found that those streams have to stay within a particular size and flow rate; otherwise, the matter would fall into the black hole in irregular clumps, causing more light fluctuation.

This close-up view of the center of the Andromeda galaxy, taken by NASA’s retired Spitzer Space Telescope, is annotated with blue dotted lines to highlight the path of two dust streams flowing toward the supermassive black hole at the galaxy’s center (indicated by a purple dot). Hi-res image

When the authors compared their findings to data from Spitzer and NASA's Hubble Space Telescope, they found spirals of dust previously identified by Spitzer that fit within these constraints. From this, the authors concluded that the spirals are feeding Andromeda's supermassive black hole.

"This is a great example of scientists reexamining archival data to reveal more about galaxy dynamics by comparing it to the latest computer simulations," said Almudena Prieto, an astrophysicist at the Institute of Astrophysics of the Canary Islands and the University Observatory Munich, and a co-author on the study published this year. "We have 20-year-old data telling us things we didn't recognize in it when we first collected it."

A Deeper Look at Andromeda

Launched in 2003 and managed by NASA's Jet Propulsion Laboratory, Spitzer studied the universe in infrared light, which is invisible to human eyes. Different wavelengths reveal different features of Andromeda, including hotter sources of light, like stars, and cooler sources, like dust.

By separating these wavelengths and looking at the dust alone, astronomers can see the galaxy's "skeleton" — places where gas has coalesced and cooled, sometimes forming dust, creating conditions for stars to form. This view of Andromeda revealed a few surprises. For instance, although it is a spiral galaxy like the Milky Way, Andromeda is dominated by a large dust ring rather than distinct arms circling its center. The images also revealed a secondary hole in one portion of the ring where a dwarf galaxy passed through.

Andromeda's proximity to the Milky Way means it looks larger than other galaxies from Earth: Seen with the naked eye, Andromeda would be about six times the width of the Moon (about 3 degrees). Even with a field of view wider than Hubble's, Spitzer had to take 11,000 snapshots to create this comprehensive picture of Andromeda.




More About the Mission

JPL managed the Spitzer Space Telescope mission for NASA's Science Mission Directorate in Washington until the mission was retired in January 2020. Science operations were conducted at the Spitzer Science Center at Caltech. Spacecraft operations were based at Lockheed Martin Space in Littleton, Colorado. Data are archived at the Infrared Science Archive operated by IPAC at Caltech. Caltech manages JPL for NASA.




News Media Contact:

Calla Cofield
Jet Propulsion Laboratory, Pasadena, Calif.
626-808-2469

calla.e.cofield@jpl.nasa.gov


Friday, May 17, 2024

Little Red Dots and Big Black Holes

Images of six "little red dot" galaxies from JWST.
Credit: NASA/ESA/CSA/I. Labbe


Title: A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields
Authors: Vasily Kokorev et al.
First Author’s Institution: Kapteyn Astronomical Institute
Status: Accepted to ApJ

Imagine you peek into a kindergarten class and, to your shock, you see that all the children are well over 6 feet tall. That is precisely how astronomers felt when data from JWST showed galaxies with massive black holes just a few hundred million years after the birth of the universe. Some of these black holes have been measured to be a million times more massive than the mass of our Sun, and astronomers are puzzled as to how they could have gained so much mass in such a short time.

The earliest galaxies likely to host these black holes show up as little red dots in the images JWST took of the early universe (as seen in the long exposure images; see the bottom image in Figure 1). They are believed to be compact (with a small radius) galaxies with a Type I active galactic nucleus and obscured (covered by dust), which accounts for their red color and why they are easily observed in the infrared. The spectrum of the galaxy has a “V” shape, a blue continuum from the unobscured part of the active galactic nucleus in the galaxy, and a red continuum from the obscured part (see Figure 1). These little red dots have appeared in several images taken by JWST, hinting that plenty of massive black holes are lurking in the early universe.

Figure 1: The characteristic spectrum of little red dots (on the left), with the compact source contributing to the dust-free blue color in the continuum (top right) and the dust-reddened part (bottom right). Adapted from Kokorev et al. 2024

Where You Look Matters!

It is vital to systematically look at these little red dot galaxies to understand how many massive black holes were in the early universe. Two factors can introduce biases in the counting of these galaxies. One is the phenomenon of cosmic variance: is JWST just preferentially looking in a direction with many little red dots, or should we expect the same number even when it looks at different parts of the universe? The other is how crowded it is in the direction in which you are observing: if you have a lot of stars in the direction you are looking, they could be misclassified as little red dots or vice versa. If you happen to have plenty of massive galaxy clusters in the direction you are looking, they may create an illusion that more of these little red dots exist than their true numbers (a phenomenon known as gravitational lensing).

To minimize the errors caused by these effects in determining the number of little red dots in the early universe, the authors of today’s research article specifically look at large areas (640 arcminutes2) of the sky by combining JWST data from various programs. This would minimize the effects of cosmic variance as you can measure the numbers over a bigger area of the sky. They also look specifically at data in blank fields (defined here as areas on the sky without galaxy clusters), which helps them determine the accurate number of objects per unit volume. All these galaxies are photometrically selected (i.e., chosen only from looking at images rather than spectra), meaning there is limited spectroscopic data to help confirm what kind of objects they are. Galaxies are determined to be little red dots based on their red colors and how compact they are in the images. Using the obtained fluxes, the authors then construct spectral energy distributions to determine the redshifts (z) of the sample. Limiting the sample to z > 4 (for the early universe), the authors end up with 260 little red dot galaxies.

Do Not Judge a Galaxy by Its Size (in Your JWST Image!)

On calculating the total luminosity of the little red dots and comparing it to their redshifts, the authors find a large number of bright little red dots at redshift of z = 5 (around a billion years after the beginning of the universe). The number of little red dots is almost 100 times more than the number of ultraviolet-selected quasars, which are active galactic nuclei identified using another method. They also find that computer models are unable to reproduce the high fraction of the bright galaxies they uncover at high redshifts (left side of Figure 2). The authors derive the mass of the black holes at redshifts of z = 4.5–6.5 to be around 106–108 solar masses, indicating that these black holes were already massive a few hundred million years after the Big Bang. They find deviations from the predicted number densities of massive black holes at these redshifts from galaxy simulations. This is likely because the galaxies that host more gigantic black holes are very dusty, and thus, their spectra do not have any blue continuum. They may then be missed from selections of little red dots as one of the factors it depends on is the characteristic “V”-shaped spectrum, which would need a contribution from the blue continuum (right side of Figure 2).

Figure 2: Left: The number density of the little red dots as a function of luminosity at 6.5 < z < 8.5 with the predicted values from simulations indicated by the blue solid line. Right: The number density as a function of black hole mass at 4.5 < z < 6.5. The observed number density of more massive black holes is lower than the values predicted by simulations. Adapted from Kokorev et al. 2024

While spectroscopy is a more reliable method to identify massive black holes, many galaxies that host black holes can still be picked out using near-infrared colors and photometry, which is a much less expensive technique. The challenge lies in ensuring that the photometrically selected sources are reliable, and the authors of today’s article made great use of this technique. Follow-up spectroscopic studies of these photometrically selected samples can help us further understand the exact nature of the black holes. Such studies are already underway, and we can look forward to finally making sense of how these black holes became so massive in such a short time after the formation of the universe!

Original astrobite edited by Delaney Dunne.




About the author, Archana Aravindan:

I am a PhD candidate at the University of California, Riverside, where I study black hole activity in small galaxies. When I am not looking through some incredible telescopes, you can usually find me reading, thinking about policy, or learning a cool language!




Editor’s Note: Astrobites is a graduate-student-run organization that digests astrophysical literature for undergraduate students. As part of the partnership between the AAS and astrobites, we occasionally repost astrobites content here at AAS Nova. We hope you enjoy this post from astrobites; the original can be viewed at astrobites.org.



Thursday, May 16, 2024

NASA's Chandra Notices the Galactic Center is Venting

Galactic Center is Venting
Credit: X-ray: NASA/CXC/Univ. of Chicago/S.C. Mackey et al.; Radio: NRF/SARAO/MeerKAT;
Image Processing: NASA/CXC/SAO/N. Wolk





These images show evidence for an exhaust vent attached to a chimney releasing hot gas from a region around the supermassive black hole at the center of the Milky Way, as reported in our latest press release. In the main image of this graphic, X-rays from NASA’s Chandra X-ray Observatory (blue) have been combined with radio data from the MeerKAT telescope (red).

Previously, astronomers had identified a “chimney” of hot gas near the Galactic Center using X-ray data from Chandra and ESA’s XMM-Newton. Radio emission detected by MeerKAT shows the effect of magnetic fields enclosing the gas in the chimney.

The evidence for the exhaust vent is highlighted in the inset, which includes only Chandra data. Several X-ray ridges showing brighter X-rays appear in white, roughly perpendicular to the plane of the Galaxy. Researchers think these are the walls of a tunnel, shaped like a cylinder, which helps funnel hot gas as it moves upwards along the chimney and away from the Galactic Center.

A labeled version of the image gives the locations of the exhaust vent, the chimney, the supermassive black hole at the center of the Milky Way Galaxy (called Sagittarius A*, or Sgr A* for short) and the plane of the galaxy.

Region Near the Milky Way's Galactic Center (Labeled).
Credit: X-ray: NASA/CXC/Univ. of Chicago/S.C. Mackey et al.; Radio: NRF/SARAO/MeerKAT;
Image Processing: NASA/CXC/SAO/N. Wolk


This newly discovered vent is located near the top of the chimney about 700 light-years from the center of the Galaxy. To emphasize the chimney and exhaust vent features the image has been rotated by 180 degrees from the conventional orientation used by astronomers, so that the chimney is pointed upwards.

The authors of the new study think that the exhaust vent formed when hot gas rising through the chimney struck cooler gas lying in its path. The brightness of the exhaust vent walls in X-rays is caused by shock waves — similar to sonic booms from supersonic planes — generated by this collision. The left side of the exhaust vent is likely particularly bright in X-rays because the gas flowing upwards is striking the tunnel wall at a more direct angle and with more force than other regions.

The researchers determined that the hot gas is most likely coming from a sequence of events involving material falling towards Sgr A*. They think eruptions from the black hole then drove the gas upwards along the chimneys, and out through the exhaust vent.

It is unclear how often material is falling onto Sgr A*. Previous studies have indicated that dramatic X-ray flares take place every few hundred years at or near the location of the central black hole, so those could play important roles in driving the hot gas upwards through the exhaust vent. Astronomers also estimate that the Galactic black hole rips apart and swallows a star every 20,000 years or so. Such events would lead to powerful, explosive releases of energy, much of which would be destined to rise through the chimney vent.

The paper describing these results is published in The Astrophysical Journal and a preprint is available online. The authors of the paper are Scott Mackey (University of Chicago), Mark Morris (University of California, Los Angeles), Gabriele Ponti (Italian National Institute of Astrophysics in Merate ), Konstantina Anastasopoulou (Italian National Institute of Astrophysics in Palermo), and Samaresh Mondal (Italian National Institute of Astrophysics in Merate).

NASA's Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory's Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.





Visual Description:

This image shows a region near the center of our Milky Way galaxy in X-ray and radio light. At the bottom of the image, near the center, is a brilliant, tangled knot of material that resembles a paint splatter. This is the brightest region in the image, and it contains the supermassive black hole at the center of our galaxy, known as Sagittarius A*.

The lower third of the image resembles an angry firestorm. Streaks of red and orange are scattered in every direction, as if a legion of embers from a fire crackled and popped into the air all at once. Flame-like structures lick toward the center from our right.

Much of the image is infused with wispy blue clouds showing X-rays detected by Chandra. At a few points, the wispy blue clouds seem to form into balls of teal colored light and are known as dust halos. They are caused by X-rays from bright X-ray sources reflecting off dust surrounding the sources. These dust halos resemble underwater lights glowing in a cloudy swimming pool at night.

Rising up from Sagittarius A* in the center of the image is a pillar of blue light referred to as a chimney. This chimney of hot gas is surrounded by red clouds that are filled with stars, presenting themselves as tiny red flecks. Near the top of the blue pillar is a streak of light blue, outlined by an illustrated, gray box. This streak is referred to as the chimney exhaust vent. Just to our left is another illustrated box that shows the close-up image of the chimney vent as observed by Chandra.




Fast Facts for Galactic Center Vent:

Scale: Large image is about 120 arcmin (900 light-years) across and the inset image is about 17 arcminutes across (130 light-years).
Category: Milky Way Galaxy, Black Holes
Coordinates (J2000): RA 17h 51m 26.3s | Dec -29° 35´ 19.4"
Constellation: Sagittarius
Observation Dates: 13 observations from Aug 22, 2005 to Aug 1, 2008 (inset image).
Observation Time: 272 hours 42 minutes (11 days 8 hours 42 minutes) (inset image)
Obs. ID: 5934, 6362, 6365, 9500-9505, 9854, 9855, 9892, 9893 (inset image)
Instrument: ACIS
References: Mackey, S.C, et. al, ApJ, 2024 (Accepted); arXiv:2310.02892
Color Code: X-ray: blue and white; Radio: orange and yellow
Distance Estimate: About 26,000 light-years


Wednesday, May 15, 2024

ONe Nova to Rule Them All

An artist's impression of this research.
Credit: NAOJ -
Download image (1.7MB)

Astronomers have proposed a new theory to explain the origin of phosphorus, one of the elements important for life on Earth. The theory suggests a type of stellar explosion known as ONe novae as a major source of phosphorus.

After the Big Bang, almost all of the matter in the Universe was comprised of hydrogen. Other elements were formed later, by nuclear reactions inside stars or when stars exploded in events known as novae or supernovae. But there are a variety of stars and a variety of ways they can explode. Astronomers are still trying to figure out which processes were important in creating the abundances of elements we see in the Universe.

In this study, Kenji Bekki, at The University of Western Australia, and Takuji Tsujimoto, at the National Astronomical Observatory of Japan, proposed a new model based on oxygen-neon novae, denoted as “ONe novae,” to explain the abundance of phosphorus. A ONe nova occurs when matter builds up on the surface of an oxygen-neon-magnesium rich white dwarf star and is heated to the point to ignite explosive run-away nuclear fusion.

The model predicts that a large amount of phosphorus will be released in a ONe nova and that the number of novae will depend on the chemical composition, specifically the iron content, of the stars. The researchers estimate that the rate of ONe novae peaked around 8 billion years ago, meaning that phosphorus would have been readily available when the Solar System started to form around 4.6 billion years ago.

The model predicts that ONe novae will produce a chlorine enhancement similar to the phosphorus enhancement. There is not yet enough observational data for chlorine to confirm this and it provides a testable hypothesis to check the validity of the ONe novae model. Future observations of stars in the outer part of the Milky Way Galaxy will provide the data needed to see if the predicted iron dependency and chlorine enhancement match reality, or if a rethink is needed.




Release Information

Researcher(s) Involved in this Release

Takuji Tsujimoto (National Astronomical Observatory of Japan)
Kenji Bekki (ICRAR, The University of Western Australia)

Coordinated Release Organization(s)

National Astronomical Observatory of Japan

Paper(s)

Kenji Bekki and Takuji Tsujimoto “Phosphorus Enhancement by ONe Novae in the Galaxy” in The Astrophysical Journal Letters, DOI: 10.3847/2041-8213/ad3fb6


Tuesday, May 14, 2024

Lenticular dust in detail

Lenticular galaxy NGC 4753 is featured with a bright white core and surrounding defined dust lanes around its nucleus, that predominantly appear dark brown in colour. A variety of faint stars fill the background of the image. Credit: ESA/Hubble & NASA, L. Kelsey. Hi-res image

Featured in this new image from the NASA/ESA Hubble Space Telescope is a nearly edge-on view of the lenticular galaxy NGC 4753. These galaxies have an elliptical shape and ill-defined spiral arms.

This image is the object's sharpest view to date, showcasing Hubble’s incredible resolving power and ability to reveal complex dust structures. NGC 4753 resides around 60 million light-years from Earth in the constellation Virgo and was first discovered by the astronomer William Herschel in 1784. It is a member of the NGC 4753 Group of galaxies within the Virgo II Cloud, which comprises roughly 100 galaxies and galaxy clusters.

This galaxy is believed to be the result of a galactic merger with a nearby dwarf galaxy roughly 1.3 billion years ago. NGC 4753’s distinct dust lanes around its nucleus are believed to have been accreted from this merger event.

It is now believed that most of the mass in the galaxy lies in a slightly flattened spherical halo of dark matter. Dark matter is a form of matter that cannot currently be observed directly, but is thought to comprise about 85% of all matter in the Universe. It is referred to as ‘dark’ because it does not appear to interact with the electromagnetic field, and therefore does not seem to emit, reflect or refract light.

This object is also of scientific interest to test different theories of formation of lenticular galaxies, given its low-density environment and complex structure. Furthermore, this galaxy has been host to two known Type Ia supernovae. These types of supernovae are extremely important as they are all caused by exploding white dwarfs which have companion stars, and always peak at the same brightness — 5 billion times brighter than the Sun. Knowing the true brightness of these events, and comparing this with their apparent brightness, gives astronomers a unique chance to measure distances in the Universe.



Monday, May 13, 2024

MIT astronomers observe elusive stellar light surrounding ancient quasars

A James Webb Telescope image shows the J0148 quasar circled in red. Two insets show, on top, the central black hole, and on bottom, the stellar emission from the host galaxy. Credits: Image: Courtesy of the researchers; NASA

MIT astronomers have observed the elusive starlight surrounding some of the earliest quasars in the universe. The distant signals, which trace back more than 13 billion years to the universe’s infancy, are revealing clues to how the very first black holes and galaxies evolved.

Quasars are the blazing centers of active galaxies, which host an insatiable supermassive black hole at their core. Most galaxies host a central black hole that may occasionally feast on gas and stellar debris, generating a brief burst of light in the form of a glowing ring as material swirls in toward the black hole.

Quasars, by contrast, can consume enormous amounts of matter over much longer stretches of time, generating an extremely bright and long-lasting ring — so bright, in fact, that quasars are among the most luminous objects in the universe.

Because they are so bright, quasars outshine the rest of the galaxy in which they reside. But the MIT team was able for the first time to observe the much fainter light from stars in the host galaxies of three ancient quasars.

Based on this elusive stellar light, the researchers estimated the mass of each host galaxy, compared to the mass of its central supermassive black hole. They found that for these quasars, the central black holes were much more massive relative to their host galaxies, compared to their modern counterparts.

The findings, published today (May 6, 2024) in the Astrophysical Journal, may shed light on how the earliest supermassive black holes became so massive despite having a relatively short amount of cosmic time in which to grow. In particular, those earliest monster black holes may have sprouted from more massive “seeds” than more modern black holes did.

“After the universe came into existence, there were seed black holes that then consumed material and grew in a very short time,” says study author Minghao Yue, a postdoc in MIT’s Kavli Institute for Astrophysics and Space Research. “One of the big questions is to understand how those monster black holes could grow so big, so fast.”

“These black holes are billions of times more massive than the sun, at a time when the universe is still in its infancy,” says study author Anna-Christina Eilers, assistant professor of physics at MIT. “Our results imply that in the early universe, supermassive black holes might have gained their mass before their host galaxies did, and the initial black hole seeds could have been more massive than today.”

Eilers’ and Yue’s co-authors include MIT Kavli Director Robert Simcoe, MIT Hubble Fellow and postdoc Rohan Naidu, and collaborators in Switzerland, Austria, Japan, and at North Carolina State University.

Dazzling cores

A quasar’s extreme luminosity has been obvious since astronomers first discovered the objects in the 1960s. They assumed then that the quasar’s light stemmed from a single, star-like “point source.” Scientists designated the objects “quasars,” as a portmanteau of a “quasi-stellar” object. Since those first observations, scientists have realized that quasars are in fact not stellar in origin but emanate from the accretion of intensely powerful and persistent supermassive black holes sitting at the center of galaxies that also host stars, which are much fainter in comparison to their dazzling cores.

It’s been extremely challenging to separate the light from a quasar’s central black hole from the light of the host galaxy’s stars. The task is a bit like discerning a field of fireflies around a central, massive searchlight. But in recent years, astronomers have had a much better chance of doing so with the launch of NASA’s James Webb Space Telescope (JWST), which has been able to peer farther back in time, and with much higher sensitivity and resolution, than any existing observatory.

In their new study, Yue and Eilers used dedicated time on JWST to observe six known, ancient quasars, intermittently from the fall of 2022 through the following spring. In total, the team collected more than 120 hours of observations of the six distant objects.

“The quasar outshines its host galaxy by orders of magnitude. And previous images were not sharp enough to distinguish what the host galaxy with all its stars looks like,” Yue says. “Now for the first time, we are able to reveal the light from these stars by very carefully modeling JWST’s much sharper images of those quasars.”

A light balance

The team took stock of the imaging data collected by JWST of each of the six distant quasars, which they estimated to be about 13 billion years old. That data included measurements of each quasar’s light in different wavelengths. The researchers fed that data into a model of how much of that light likely comes from a compact “point source,” such as a central black hole’s accretion disk, versus a more diffuse source, such as light from the host galaxy’s surrounding, scattered stars.

Through this modeling, the team teased apart each quasar’s light into two components: light from the central black hole’s luminous disk and light from the host galaxy’s more diffuse stars. The amount of light from both sources is a reflection of their total mass. The researchers estimate that for these quasars, the ratio between the mass of the central black hole and the mass of the host galaxy was about 1:10. This, they realized, was in stark contrast to today’s mass balance of 1:1,000, in which more recently formed black holes are much less massive compared to their host galaxies.

“This tells us something about what grows first: Is it the black hole that grows first, and then the galaxy catches up? Or is the galaxy and its stars that first grow, and they dominate and regulate the black hole’s growth?” Eilers explains. “We see that black holes in the early universe seem to be growing faster than their host galaxies. That is tentative evidence that the initial black hole seeds could have been more massive back then.”

“There must have been some mechanism to make a black hole gain their mass earlier than their host galaxy in those first billion years,” Yue adds. “It’s kind of the first evidence we see for this, which is exciting.”
 
Jennifer Chu | MIT News 



Sunday, May 12, 2024

NASA's Roman Space Telescope Could Help Researchers Detect the Universe’s First Stars

Tidal Disruption of a Star (Artist’s Concept)
Credits: Illustration: Ralf Crawford (STScI)




The first stars to form in the universe were very different from our Sun. Known to astronomers (somewhat paradoxically) as Population III, or Pop III, stars, they were made almost entirely of hydrogen and helium. They are believed to have been much larger, hotter, and more massive than our Sun. As a result, Pop III stars use their fuel more quickly and have shorter lifespans.

Pop III stars, which came about in the first few hundred million years after the big bang, are crucial in understanding the development of the universe. These stars were the nuclear furnaces where the first elements heavier than helium, which astronomers call metals, were generated, and ultimately are the reason for the complex systems of galaxies in the current universe.

No Pop III stars are found around us today, so to learn about them we must look back to the early universe. NASA’s Nancy Grace Roman Space Telescope will provide a panoramic field of view 200 times larger than the infrared view of the sky from NASA’s Hubble Space Telescope and survey the sky 1,000 times faster. As a result, Roman may be a key tool for helping astronomers see this rare first generation of stars after it launches by May 2027.

Shredded Stars

The new approach will not seek intact stars. Instead, astronomers will hunt for signs of Pop III stars that have been shredded by black holes, creating a bright and energetic phenomenon known as a tidal disruption event (TDE).

If a star moves close enough to a black hole, the star will experience gravitational tides strong enough to completely disrupt it. Some of the material from the disrupted star then collects into an accretion disk, where complex physical processes cause it to glow brightly enough to be seen from billions of light-years away.

"Since we know that black holes likely exist at these early epochs, catching them as they’re devouring these first stars might offer us the best shot to indirectly detect Pop III stars," noted Priyamvada Natarajan of Yale University, a co-author of the study.

TDEs generate light in many wavelengths, including X-ray, radio, ultraviolet (UV), and optical light. The further we look into the early universe, where these early stars primarily reside, the more the optical and UV light is redshifted, or stretched by the expanding universe, into near-infrared wavelengths visible to Roman.

Not only does the wavelength of light stretch – so does the observed timescale of the TDE. Like an exploding star or supernova, a TDE is a transient event that increases quickly in brightness and then gradually decreases over time. But due to the large redshift of these events, a Pop III TDE would brighten over the course of hundreds to thousands of days, while its decline would last more than a decade.

“The evolution timescales of Pop III TDEs are very long, which is one feature that could distinguish a Pop III TDE from other transients including supernovas and TDEs of current-generation stars like our Sun,” said Rudrani Kar Chowdhury, postdoctoral fellow of the University of Hong Kong and first author of the study.

“Since they last for a longer time, a Pop III TDE might be easier to detect, but it might be harder to identify as a transient,” added co-author Jane Dai, professor of astrophysics at the University of Hong Kong. “Scientists would need to design the right survey strategy.”

A Coordinated Hunt

While NASA’s James Webb Space Telescope is powerful enough to detect and study TDEs in the early universe, its field of view is too small to make it an efficient TDE hunter. Of Roman’s core community surveys, the most promising for finding TDEs is the High Latitude Wide Area survey, which aims to cover approximately 2,000 square degrees of the sky outside of the plane of our galaxy.

“Roman can go very deep and yet cover a very big area of the sky. That's what's needed to detect a meaningful sample of these TDEs,” said Dai.

Webb would be useful for follow-up observations, however, particularly with its suite of spectroscopic tools. Once Roman detects these TDEs, Webb’s instruments could identify if any metals are present.

“Since these stars are only made up of hydrogen and helium, we will not see any metal lines in the spectrum of objects, whereas in the spectra of TDEs from regular stars we can see various metal lines,” Kar Chowdhury noted.

With this proposed strategy for identifying Pop III stars, there’s an opportunity to explore more of the universe’s mysteries, opening up numerous opportunities to better understand not only the early universe, but also galaxies closer to home.

This research has been published in the Astrophysical Journal Letters.

The Nancy Grace Roman Space Telescope is managed at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, with participation by NASA's Jet Propulsion Laboratory and Caltech/IPAC in Southern California, the Space Telescope Science Institute in Baltimore, and a science team comprising scientists from various research institutions. The primary industrial partners are BAE Systems, Inc. in Boulder, Colorado; L3Harris Technologies in Melbourne, Florida; and Teledyne Scientific & Imaging in Thousand Oaks, California.




About This Release

Credits:

Media Contact:

Matthew Brown
Space Telescope Science Institute, Baltimore, Maryland

Christine Pulliam
Space Telescope Science Institute, Baltimore, Maryland

Science: Jane Dai (University of Hong Kong), Rudrani Kar Chowdhury (University of Hong Kong)

Permissions: Content Use Policy

Related Links and Documents


NASA, JAXA XRISM Spots Iron Fingerprints in Nearby Active Galaxy

The Resolve instrument aboard XRISM (X-ray Imaging and Spectroscopy Mission) captured data from the center of galaxy NGC 4151, where a supermassive black hole is slowly consuming material from the surrounding accretion disk. The resulting spectrum reveals the presence of iron in the peak around 6.5 keV and the dips around 7 keV, light thousands of times more energetic that what our eyes can see. Background: An image of NGC 4151 constructed from a combination of X-ray, optical, and radio light. Spectrum: JAXA/NASA/XRISM Resolve. Background: X-rays, NASA/CXC/CfA/J.Wang et al.; optical, Isaac Newton Group of Telescopes, La Palma/Jacobus Kapteyn Telescope; radio, NSF/NRAO/VLA

After starting science operations in February, Japan-led XRISM (X-ray Imaging and Spectroscopy Mission) studied the monster black hole at the center of galaxy NGC 4151.

“XRISM’s Resolve instrument captured a detailed spectrum of the area around the black hole,” said Brian Williams, NASA’s project scientist for the mission at the agency’s Goddard Space Flight Center in Greenbelt, Maryland. “The peaks and dips are like chemical fingerprints that can tell us what elements are present and reveal clues about the fate of matter as it nears the black hole.”

XRISM (pronounced “crism”) is led by JAXA (Japan Aerospace Exploration Agency) in collaboration with NASA, along with contributions from ESA (European Space Agency). It launched Sept. 6, 2023. NASA and JAXA developed Resolve, the mission’s microcalorimeter spectrometer.

NGC 4151 is a spiral galaxy around 43 million light-years away in the northern constellation Canes Venatici. The supermassive black hole at its center holds more than 20 million times the Sun’s mass.

The galaxy is also active, which means its center is unusually bright and variable. Gas and dust swirling toward the black hole form an accretion disk around it and heat up through gravitational and frictional forces, creating the variability. Some of the matter on the brink of the black hole forms twin jets of particles that blast out from each side of the disk at nearly the speed of light. A puffy donut-shaped cloud of material called a torus surrounds the accretion disk.

In fact, NGC 4151 is one of the closest-known active galaxies. Other missions, including NASA’s Chandra X-ray Observatory and Hubble Space Telescope, have studied it to learn more about the interaction between black holes and their surroundings, which can tell scientists how supermassive black holes in galactic centers grow over cosmic time.

This artist’s concept shows the possible locations of iron revealed in XRISM’s X-ray spectrum of NGC 4151. Scientists think X-ray-emitting iron is in the hot accretion disk, close to the black hole. The X-ray-absorbing iron may be further away, in a cooler cloud of material called a torus. NASA's Goddard Space Flight Center Conceptual Image Lab.

The galaxy is uncommonly bright in X-rays, which made it an ideal early target for XRISM.

Resolve’s spectrum of NGC 4151 reveals a sharp peak at energies just under 6.5 keV (kiloelectron volts) — an emission line of iron. Astronomers think that much of the power of active galaxies comes from X-rays originating in hot, flaring regions close to the black hole. X-rays bouncing off cooler gas in the disk causes iron there to fluoresce, producing a specific X-ray peak. This allows astronomers to paint a better picture of both the disk and erupting regions much closer to the black hole.

The spectrum also shows several dips around 7 keV. Iron located in the torus caused these dips as well, although through absorption of X-rays, rather than emission, because the material there is much cooler than in the disk. All this radiation is some 2,500 times more energetic than the light we can see with our eyes.

Iron is just one element XRISM can detect. The telescope can also spot sulfur, calcium, argon, and others, depending on the source. Each tells astrophysicists something different about the cosmic phenomena scattered across the X-ray sky.

XRISM is a collaborative mission between JAXA and NASA, with participation by ESA. NASA’s contribution includes science participation from CSA (Canadian Space Agency).

Download high-resolution images on NASA's Scientific Visualization Studio

By Jeanette Kazmierczak
NASA’s Goddard Space Flight Center, Greenbelt, Md.



Media Contact:

Claire Andreoli
301-286-1940

claire.andreoli@nasa.gov
NASA’s Goddard Space Flight Center, Greenbelt, Md.



Saturday, May 11, 2024

NASA's Webb Hints at Possible Atmosphere Surrounding Rocky Exoplanet

Super-Earth Exoplanet 55 Cancri e (Artist’s Concept)
Credits: Illustration: NASA, ESA, CSA, Ralf Crawford (STScI)

Super-Earth Exoplanet 55 Cancri e (MIRI Secondary Eclipse Light Curve)
Credits: Illustration: NASA, ESA, CSA, Joseph Olmsted (STScI)
Science: Aaron Bello-Arufe (NASA-JPL)

Super-Earth Exoplanet 55 Cancri e (NIRCam + MIRI Emission Spectrum)
Credits: Illustration: NASA, ESA, CSA, Joseph Olmsted (STScI)
Science: Renyu Hu (NASA-JPL), Aaron Bello-Arufe (NASA-JPL), Michael Zhang (University of Chicago), Mantas Zilinskas (SRON)



Researchers using NASA’s James Webb Space Telescope may have detected atmospheric gases surrounding 55 Cancri e, a hot rocky exoplanet 41 light-years from Earth. This is the best evidence to date for the existence of any rocky planet atmosphere outside our solar system.

Renyu Hu from NASA’s Jet Propulsion Laboratory (JPL) in Pasadena, California, is lead author on a paper published today in Nature. “Webb is pushing the frontiers of exoplanet characterization to rocky planets,” Hu said. “It is truly enabling a new type of science.”

Super-Hot Super-Earth 55 Cancri e

55 Cancri e, also known as Janssen, is one of five known planets orbiting the Sun-like star 55 Cancri, in the constellation Cancer. With a diameter nearly twice that of Earth and density slightly greater, the planet is classified as a super-Earth: larger than Earth, smaller than Neptune, and likely similar in composition to the rocky planets in our solar system.

To describe 55 Cancri e as “rocky,” however, could leave the wrong impression. The planet orbits so close to its star (about 1.4 million miles, or one-twenty-fifth the distance between Mercury and the Sun) that its surface is likely to be molten – a bubbling ocean of magma. With such a tight orbit, the planet is also likely to be tidally locked, with a dayside that faces the star at all times and a nightside in perpetual darkness.

In spite of numerous observations since it was discovered to transit in 2011, the question of whether or not 55 Cancri e has an atmosphere – or even could have one given its high temperature and the continuous onslaught of stellar radiation and wind from its star – has gone unanswered.

“I’ve worked on this planet for more than a decade,” said Diana Dragomir, an exoplanet researcher at the University of New Mexico and co-author on the study. “It’s been really frustrating that none of the observations we’ve been getting have robustly solved these mysteries. I am thrilled that we're finally getting some answers!”

Unlike the atmospheres of gas giant planets, which are relatively easy to spot (the first was detected by NASA’s Hubble Space Telescope more than two decades ago), thinner and denser atmospheres surrounding rocky planets have remained elusive.

Previous studies of 55 Cancri e using data from NASA’s now-retired Spitzer Space Telescope suggested the presence of a substantial atmosphere rich in volatiles (molecules that occur in gas form on Earth) like oxygen, nitrogen, and carbon dioxide. But researchers could not rule out another possibility: that the planet is bare, save for a tenuous shroud of vaporized rock, rich in elements like silicon, iron, aluminum, and calcium. “The planet is so hot that some of the molten rock should evaporate,” explained Hu.

Measuring Subtle Variations in Infrared Colors

To distinguish between the two possibilities, the team used Webb’s NIRCam (Near-Infrared Camera) and MIRI (Mid-Infrared Instrument) to measure 4- to 12-micron infrared light coming from the planet.

Although Webb cannot capture a direct image of 55 Cancri e, it can measure subtle changes in light from the system as the planet orbits the star.

By subtracting the brightness during the secondary eclipse, when the planet is behind the star (starlight only), from the brightness when the planet is right beside the star (light from the star and planet combined), the team was able to calculate the amount of various wavelengths of infrared light coming from the dayside of the planet.

This method, known as secondary eclipse spectroscopy, is similar to that used by other research teams to search for atmospheres on other rocky exoplanets, like TRAPPIST-1 b.

Cooler than Expected

The first indication that 55 Cancri e could have a substantial atmosphere came from temperature measurements based on its thermal emission, or heat energy given off in the form of infrared light. If the planet is covered in dark molten rock with a thin veil of vaporized rock or no atmosphere at all, the dayside should be around 4,000 degrees Fahrenheit (~2,200 degrees Celsius).

“Instead, the MIRI data showed a relatively low temperature of about 2,800 degrees Fahrenheit [~1540 degrees Celsius],” said Hu. “This is a very strong indication that energy is being distributed from the dayside to the nightside, most likely by a volatile-rich atmosphere.” While currents of lava can carry some heat around to the nightside, they cannot move it efficiently enough to explain the cooling effect.

When the team looked at the NIRCam data, they saw patterns consistent with a volatile-rich atmosphere. “We see evidence of a dip in the spectrum between 4 and 5 microns — less of this light is reaching the telescope,” explained co-author Aaron Bello-Arufe, also from NASA JPL. “This suggests the presence of an atmosphere containing carbon monoxide or carbon dioxide, which absorb these wavelengths of light.” A planet with no atmosphere or an atmosphere consisting only of vaporized rock would not have this specific spectral feature.

“We’ve spent the last ten years modelling different scenarios, trying to imagine what this world might look like,” said co-author Yamila Miguel from the Leiden Observatory and the Netherlands Institute for Space Research (SRON). “Finally getting some confirmation of our work is priceless!”

Bubbling Magma Ocean

The team thinks that the gases blanketing 55 Cancri e would be bubbling out from the interior, rather than being present ever since the planet formed. “The primary atmosphere would be long gone because of the high temperature and intense radiation from the star,” said Bello-Arufe. “This would be a secondary atmosphere that is continuously replenished by the magma ocean. Magma is not just crystals and liquid rock; there’s a lot of dissolved gas in it, too.”

While 55 Cancri e is far too hot to be habitable, researchers think it could provide a unique window for studying interactions between atmospheres, surfaces, and interiors of rocky planets, and perhaps provide insights into the early conditions of Earth, Venus, and Mars, which are thought to have been covered in magma oceans far in the past. “Ultimately, we want to understand what conditions make it possible for a rocky planet to sustain a gas-rich atmosphere: a key ingredient for a habitable planet,” said Hu. This research was conducted as part of Webb’s General Observers (GO) Program 1952. Analysis of additional secondary eclipse observations of 55 Cancri e are currently in progress.

The James Webb Space Telescope is the world’s premier space science observatory. Webb is solving mysteries in our solar system, looking beyond to distant worlds around other stars, and probing the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency) and the Canadian Space Agency.




About This Release

Credits:

Media Contact:

Margaret W. Carruthers
Space Telescope Science Institute, Baltimore, Maryland

Christine Pulliam
Space Telescope Science Institute, Baltimore, Maryland

Science: Renyu Hu (NASA-JPL)

Permissions: Content Use Policy

 Contact Us: Direct inquiries to the News Team.

Related Links and Documents


Friday, May 10, 2024

A Vampire’s Sandwich Filled with Gas and Dust Jennifer Chu | MIT News

These images show the serendipitously discovered protoplanetary disk named Dracula's Chivito
Adapted from Breghea et al. 2024


The observations suggest some of earliest “monster” black holes grew from massive cosmic seeds.

Title: Dracula’s Chivito: Discovery of a Large Edge-On Protoplanetary Disk with Pan-STARRS
Authors: Ciprian T. Berghea et al.
First Author’s Institution: US Naval Observatory
Status: Accepted to ApJL

Where Planets Are Born

Studying protoplanetary disks helps us understand how planets, including those in our solar system, are born. These disks are vast and flared structures, consisting of dust and gas orbiting a young star. Protoplanetary disks contain the remnants of the stellar birth process, in which a collapsing molecular cloud gives rise to a central star surrounded by a swirling disk of material. Protoplanetary disks are vital to observe as they are the birth sites of planets. The tiny dust particles come together, sticking to each other and forming larger bodies. This process, influenced by gravity, gas, and radiation, leads to the birth of planets in developing planetary systems.

Meet the Vampire Sub

This research article features a large edge-on protoplanetary disk that was stumbled upon when going through images from the Pan-STARRS research project as a part of a study of active galactic nucleus candidates. This disk is one of the largest known disks in the sky and is oriented edge on, completely obscuring its central star. Associated with a source of infrared light in the same region of the sky, IRAS 23077+6707, the disk spans approximately 11″ in apparent size, with a very faint structure in the disk’s northern part extending out to about 17″. It is possibly the largest protoplanetary disk (by angular extent) discovered to date. The structure of this disk is reminiscent of the popular Gomez’s Hamburger, which is not associated with any star-forming region, just like the subject of this article. The similarity to a sandwich, along with the fang-like structures in the northern part of the disk as seen in the images in Figure 1, earned the IRAS 23077+6707 protoplanetary disk the name “Dracula’s Chivito” (chivito is a type of sandwich and the national dish of Uruguay, where one of the co-authors is from).

Decoding DraChi

Analysis: Images of Dracula’s Chivito (henceforth referred to as DraChi) were obtained in the grizy filters of Pan-STARRS (Figure 1). These images and data from the Galaxy Evolution Explorer (GALEX) (ultraviolet), the Two Micron All-Sky Survey (2MASS) (infrared), the Infrared Astronomical Satellite (IRAS) (infrared), and AKARI (infrared) were used for photometric analysis, i.e., flux or brightness measurements. These data were used to construct the spectral energy distribution of the disk (Figure 2), together with a radiative transfer model generated using the code HOCHUNK3D. Radiative transfer models help us understand the disk geometry and how light is scattered by the dust grains in the disk. This light, which we see along our line of sight, is plotted as a spectral energy distribution. Spectral energy distributions give information about how much energy an object gives off at different wavelengths.

Figure 2: The spectral energy distribution of the disk, using photometric data from the image, the model, and other sources as mentioned in the article. Brightness is plotted as a function of wavelength. The data (colored dots) match the model (the solid red line shows the model without extinction, and the dashed red line shows the model with extinction) in most places except in near- and mid-infrared wavelengths, which could be due to discrepancies between instruments or possible variability in the disk’s luminosity. Berghea et al. 2024

Distance: It is hard to estimate DraChi’s distance because it is not associated with a known star-forming region. Accurate distances to local molecular clouds are vital to locating protoplanetary disks and comprehending planet formation processes. Therefore, using the Gaia DR3 data for nearby stars, the extinction of the disk was estimated to find the distance to the nearest interstellar clouds, and DraChi is hence estimated to be 978 light-years away.

Basic Properties: The spectral energy distribution suggests that the host star of the disk is a pre-main-sequence star of type A with a temperature of about 6500–8500K. The images of the disk and the resultant radiative transfer model constrain the disk inclination to be between 80° and 84°. The scale height of the disk is about 25–50 au at a radius of 500 au (astronomical units), where 1 au is the distance from Earth to the Sun. Using the distance and the angular extent of the disk in the sky, the disk’s radius is estimated to be 1,650 au. The radiative transfer model, based on the scattering of the light, quantifies the mass of the disk to be about 0.2 times that of the Sun.

The Fangs: The authors noticed two “fang-like” features in the northern part of the disk, and these features were also reproduced in the model of the disk. The “fangs” closely resemble the “edge” of the shadow created by the disk in the bright surrounding envelope. They could be filaments due to a possible outflow from the central part of the disk, which is characteristic of a young disk at the end of the Class I phase (~0.5 million years old). It is possible that the fangs are present in the south, but this region is likely obscured in the images from Pan-STARRS and could be perhaps seen in infrared (longer-wavelength) imaging.

Is DraChi the Only One?

The short answer is no. DraChi is certainly different from most other protoplanetary disks, given its size and large distance from any known star-forming regions. But the existence of Gomez’s Hamburger proves there are more such disks awaiting discovery. A disk as young as DraChi is vital to understanding planet formation in its earlier stages, and its large size makes for interesting future observations using more sensitive instruments.

Original astrobite edited by Kylee Carden and Jessie Thwaites.




About the author, Maria Vincent:

Maria is a PhD candidate in astronomy at the Institute for Astronomy, University of Hawai’i at Manoa. Her research focuses on adaptive optics and high-contrast imaging science and instrumentation with ground-based telescopes. Driven by a fascination with planet formation and the intricate processes shaping our solar system, she uses the Subaru Coronagraphic Extreme Adaptive Optics suite to observe and study morphological features of protoplanetary disks in near-infrared wavelengths, aiming to understand disk structure and processes governing planet formation. On the instrumentation side, she is working on designing and constructing an optical testbed to test and characterize a new deformable mirror as part of the upcoming High-order Advanced Keck Adaptive Optics upgrade. Outside of work, she enjoys blogging, mystery, historical and science fiction literature and cinemedia, photography, hiking, and travel.



Editor’s Note: Astrobites is a graduate-student-run organization that digests astrophysical literature for undergraduate students. As part of the partnership between the AAS and astrobites, we occasionally repost astrobites content here at AAS Nova. We hope you enjoy this post from astrobites; the original can be viewed at astrobites.org.