Podcasts about small magellanic cloud

Fireworks will light up the skies of many cities and towns this week – celebrations of Independence Day. For a real fireworks display, though, you might want to visit one of the Milky Way’s companion galaxies. It’s giving birth to many thousands of new stars, including some of the biggest and brightest yet seen anywhere – a result not of independence, but of a close relationship with another galaxy. The Large Magellanic Cloud is too far south to see from the continental United States. In southern-hemisphere skies, though, it’s quite a sight – a bright cloud that’s several times bigger than the full Moon. The galaxy is much smaller and fainter than the Milky Way. But it’s right next door – just 160,000 light-years away. That’s one of the reasons it looks so bright. Another is that the galaxy contains millions of hot young stars – stars that are thousands of times brighter than the Sun. And it’s giving birth to more. In fact, it contains a stellar nursery that’s far more impressive than anything in the Milky Way. We’ll have more about that tomorrow. The fireworks probably are the result of an interaction with another galaxy, the Small Magellanic Cloud. The smaller galaxy passed close to the bigger one. That encounter squeezed giant clouds of gas and dust. The clouds split into smaller clumps, which gave birth to new stars – creating fireworks in a busy galaxy. Script by Damond Benningfield

Astronomy Daily | Space News: S04E87In this episode of Astronomy Daily, host Anna takes you on an exhilarating journey through the latest cosmic discoveries and developments that are reshaping our understanding of the universe. From galactic drama to groundbreaking lunar exploration, this episode is packed with insights that will ignite your curiosity about the cosmos.Highlights:- Galactic Drama in the Magellanic Clouds: Join us as we explore new research suggesting that the Large Magellanic Cloud may be tearing apart its smaller companion, the Small Magellanic Cloud. Using data from the Gaia Space Telescope, scientists reveal how massive stars within the SMC are being influenced by the gravitational forces of the LMC, offering a unique perspective on cosmic interactions.- Fram 2 Mission Insights: Hear firsthand accounts from the crew of the Fram 2 mission, the first humans to orbit Earth's poles. Discover their surprising experiences and the scientific experiments conducted during this groundbreaking journey, including their observations of the auroras from a polar orbit.- China's Lunar 3D Printing Plans: Learn about China's ambitious plans to 3D print building materials on the Moon using lunar soil. Scheduled for launch in 2028, this innovative technology aims to pave the way for sustainable lunar exploration and habitation, significantly reducing reliance on Earth-sourced materials.- James Webb's Stellar Discovery: Explore the groundbreaking findings from the James Webb Space Telescope, which has observed a star consuming a planet in a remarkable cosmic event. This discovery challenges previous theories and provides new insights into the life cycle of stars and their planetary systems.- Innovative Subsurface Robots for Lunar Exploration: Delve into the concept of autonomous subsurface robots designed to explore beneath the Moon's surface. These innovative machines could uncover valuable resources and help establish infrastructure for future lunar missions.For more cosmic updates, visit our website at astronomydaily.io. Join our community on social media by searching for #AstroDailyPod on Facebook, X, YouTubeMusic, TikTok, and our new Instagram account! Don't forget to subscribe to the podcast on Apple Podcasts, Spotify, iHeartRadio, or wherever you get your podcasts.Thank you for tuning in. This is Anna signing off. Until next time, keep looking up and stay curious about the wonders of our universe.00:00 - Welcome to Astronomy Daily01:05 - Large Magellanic Cloud's impact on Small Magellanic Cloud10:30 - Fram 2 mission crew experiences17:00 - China's lunar 3D printing technology22:15 - James Webb's discovery of a star consuming a planet27:30 - Subsurface robots for lunar exploration✍️ Episode ReferencesMagellanic Clouds Research[Nagoya University](https://www.nagoya-u.ac.jp/)Fram 2 Mission Details[SpaceX](https://www.spacex.com/)China's Lunar Plans[China National Space Administration](https://www.cnsa.gov.cn/)James Webb Discoveries[NASA](https://www.nasa.gov)Lunar Exploration Robots[Planetary Exploration Research](https://www.planetary.org/)Astronomy Daily[Astronomy Daily](http://www.astronomydaily.io/)Become a supporter of this podcast: https://www.spreaker.com/podcast/astronomy-daily-exciting-space-discoveries-and-news--5648921/support.

The Small Magellanic Cloud is a satellite galaxy of the Milky Way. It's about 200,000 light-years away, it contains hundreds of millions of stars, and it's easily visible to the eye alone — from the southern hemisphere. And it may actually consist of two separate but related halves — two galaxies for the price of one. Astronomers had suggested that possibility almost four decades ago. And a recent study provided the best evidence yet to support the idea. It found two large star-forming regions that are separated by about 15,000 light-years. One lines up in front of the other, making it hard to see them as individual objects. A team studied the galaxy in several ways. It found that gas and dust are split into two distinct regions. Their material moves in different ways, and has a different composition. The researchers also studied hot, young, bright stars. That also revealed two separate regions. And like the gas, the stars in the regions move in different ways, and have a slightly different makeup. The team said the two regions could be remnants of two galaxies that came together long ago. On the other hand, the region that's closer to us could be the main body of the galaxy. The region behind it then could be a tail of stars and gas pulled out by the gravity of the nearby Large Magellanic Cloud, which is bigger and heavier. Either way, this close companion to the Milky Way may be more than meets the eye. Script by Damond Benningfield

**Host:** Stuart Gary **Special Guest:** Technology Editor Alex Zaharov-Reutt ### Episode Highlights:1. **The Dual Nature of the Small Magellanic Cloud**: New research suggests that what was previously thought to be a single galaxy, the Small Magellanic Cloud, is actually two distinct galaxies. This groundbreaking discovery, based on studies of stellar motion and the interstellar medium, challenges previous astronomical beliefs.2. **The Dwarf Planet Eris's Unexpected Composition**: A recent study has indicated that Eris, a distant dwarf planet, might possess a more 'squishy' internal structure than previously assumed. This insight opens new avenues in understanding the formation and composition of such celestial bodies.3. **NASA's PACE Satellite Launch Update**: The launch date for NASA's new PACE satellite is now scheduled for February 6th. This mission is expected to provide significant insights into oceanic ecosystems and atmospheric phenomena. ### In-Depth Analysis: -**Exploring the Magellanic Clouds**: The episode delves into the history and importance of the Large and Small Magellanic Clouds. These satellite dwarf galaxies, named after the explorer Ferdinand Magellan, have played a crucial role in navigation and astronomical studies. -**The Study of the Small Magellanic Cloud**: Utilizing data from the European Space Agency's Gaia spacecraft and the Australian Square Kilometer Array Pathfinder radio telescope, astronomers have uncovered surprising differences in chemical composition and star velocities within the Small Magellanic Cloud. -**Eris and Its Moon Dysnomia**: Discussions include the intriguing relationship between Eris and its moon Dysnomia, focusing on their tidal interactions and implications for understanding planetary structures. ### Other Topics Covered: - NASA's PACE satellite mission details and objectives. - The historical significance of the Magellanic Clouds in astronomy and navigation. - The role of the Magellanic Clouds in current astronomical research. ### Final Thoughts: The episode concludes with a reflection on the continuous advancements in space exploration and astronomical research, emphasizing the importance of such discoveries in broadening our understanding of the universe.Your support is needed... **Support SpaceTime with Stuart Gary: Be Part of Our Cosmic Journey!** SpaceTime is fueled by passion, not big corporations or grants. We're on a mission to become 100% listener-supported, allowing us to focus solely on bringing you riveting space stories without the interruption of ads.

The stars of the binary system SSN 7 are doomed, doomed, and doomed. Each of the two monster stars will collapse to form a black hole. And in the far-distant future, the black holes will merge to form a bigger one. The system is about 200,000 light-years from Earth. It's in a massive stellar nursery in the Small Magellanic Cloud, a companion galaxy to the Milky Way. A recent study found that one star in the system is about 32 time the mass of the Sun, while the other is 55 times the Sun's mass. That makes them some of the hottest, brightest, and heaviest stars in the universe. They're only about four million years old — about one percent the age of the Sun. But because they're so massive, they're nearing the ends of their lives. The study concluded that the stars are so close together that they're touching each other. Not only that, but the heavier star is “stealing” hot gas from its companion. In as little as 700,000 years, the less-massive star will collapse to form a black hole. After a brief quiet period, it will begin pulling in gas from the surviving star, which will collapse as well. The entire scenario should play out in just a few million years. After that, the black holes will spiral ever closer as they emit gravitational waves — “ripples” in space-time. The study forecasts that they'll merge in about 18 billion years — several billion years longer than the current age of the universe.  Script by Damond Benningfield Support McDonald Observatory

A giant stellar nursery in a nearby galaxy is giving birth to thousands of new stars. That includes some of the more massive stars ever seen, which will explode as supernovas. But most of the stars are much smaller and more sedate, so they'll live long, quiet lives. NGC 346 is 200,000 light-years away. It's the biggest and brightest star-forming region in the Small Magellanic Cloud -- a close companion to our home galaxy, the Milky Way. The nursery probably is about three million years old, yet it may already contain tens of thousands of stars. It probably also contains thousands of stellar wannabes -- objects that have not yet lit the fires of nuclear fusion, allowing them to shine as true stars. Until recently, astronomers had seen only the brightest and most massive of the stars that are still being born. But using James Webb Space Telescope, they found hundreds more. Most of them will form stars that are similar to the Sun or smaller. It's the first time we've ever seen the birth process of such modest stars in any galaxy beyond the Milky Way. Webb discovered dust in the disks of material around the newly forming stars -- also a first. The dust grains are made of heavy elements that could someday form planets around the stars -- especially small, rocky planets like Earth. So NGC 346 could be showing us the birth not only of thousands of future stars, but of thousands of future planets as well.  Script by Damond Benningfield Support McDonald Observatory

New calculations show how large impacts onto Mars may have boosted its greenhouse effect, helping explain how it was warm enough for all those rivers and lakes billions of years ago. If that explains Mars' early warm climate, it could be bad news for potential for life there. Futher from home, dust has been observed star forming regions in the Small Magellanic Cloud where the abundance of planet-building raw materials is low. Check out these stories, space news, and special top quark trivia.

Newly discovered Ca II absorbers in the early universe: statistics, element abundances and dust by Hannah Fang et al. on Friday 25 November We report discoveries of 165 new quasar Ca II absorbers from the Sloan Digital Sky Survey (SDSS) Data Release 7 and 12. Our Ca II rest frame equivalent width distribution supports the weak and strong subpopulations, split at ${W}^{lambda3934}_{0}=0.7${AA}. Comparison of both populations' dust depletion shows clear consistency for weak absorber association with halo-type gas in the Milky Way (MW) while strong absorbers have environments consistent with halo and disc-type gas. We probed our high redshift Ca II absorbers for 2175{AA} dust bumps, discovering 12 2175{AA} dust absorbers (2DAs). This clearly shows that some Ca II absorbers follow the Large Magellanic Cloud (LMC) extinction law rather than the Small Magellanic Cloud extinction law. About 33% of our strong Ca II absorbers exhibit the 2175{AA} dust bump while only 6% of weak Ca II absorbers show this bump. 2DA detection further supports the theory that strong Ca II absorbers are associated with disk components and are dustier than the weak population. Comparing average Ca II absorber dust depletion patterns to that of Damped Ly{alpha} Absorbers (DLAs), Mg II absorbers, and 2DAs shows that Ca II absorbers generally have environments with more dust than DLAs and Mg II absorbers, but less dust than 2DAs. Comparing 2175{AA} dust bump strengths from different samples and also the MW and LMC, the bump strength appears to grow stronger as the redshift decreases, indicating dust growth and the global chemical enrichment of galaxies in the universe over time. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13166v1

Newly discovered Ca II absorbers in the early universe: statistics, element abundances and dust by Hannah Fang et al. on Thursday 24 November We report discoveries of 165 new quasar Ca II absorbers from the Sloan Digital Sky Survey (SDSS) Data Release 7 and 12. Our Ca II rest frame equivalent width distribution supports the weak and strong subpopulations, split at ${W}^{lambda3934}_{0}=0.7${AA}. Comparison of both populations' dust depletion shows clear consistency for weak absorber association with halo-type gas in the Milky Way (MW) while strong absorbers have environments consistent with halo and disc-type gas. We probed our high redshift Ca II absorbers for 2175{AA} dust bumps, discovering 12 2175{AA} dust absorbers (2DAs). This clearly shows that some Ca II absorbers follow the Large Magellanic Cloud (LMC) extinction law rather than the Small Magellanic Cloud extinction law. About 33% of our strong Ca II absorbers exhibit the 2175{AA} dust bump while only 6% of weak Ca II absorbers show this bump. 2DA detection further supports the theory that strong Ca II absorbers are associated with disk components and are dustier than the weak population. Comparing average Ca II absorber dust depletion patterns to that of Damped Ly{alpha} Absorbers (DLAs), Mg II absorbers, and 2DAs shows that Ca II absorbers generally have environments with more dust than DLAs and Mg II absorbers, but less dust than 2DAs. Comparing 2175{AA} dust bump strengths from different samples and also the MW and LMC, the bump strength appears to grow stronger as the redshift decreases, indicating dust growth and the global chemical enrichment of galaxies in the universe over time. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13166v1

The Dual Role of Outflows in Quenching Satellites of Low-Mass Hosts: NGC 3109 by Christopher T. Garling et al. on Tuesday 20 September While dwarf galaxies observed in the field are overwhelmingly star-forming, dwarf galaxies in environments as dense or denser than the Milky Way are overwhelmingly quenched. In this paper, we explore quenching in the lower density environment of the Small-Magellanic-Cloud-mass galaxy NGC 3109 ($text{M}_* sim 10^8 , text{M}_odot$), which hosts two known dwarf satellite galaxies (Antlia and Antlia B), both of which are HI deficient compared to similar galaxies in the field and have recently stopped forming stars. Using a new semi-analytic model in concert with the measured star formation histories and gas masses of the two dwarf satellite galaxies, we show that they could not have been quenched solely by direct ram pressure stripping of their interstellar media, as is common in denser environments. Instead, we find that separation of the satellites from pristine gas inflows, coupled with stellar-feedback-driven outflows from the satellites (jointly referred to as the starvation quenching model), can quench the satellites on timescales consistent with their likely infall times into NGC 3109's halo. It is currently believed that starvation is caused by "weak" ram pressure that prevents low-density, weakly-bound gas from being accreted onto the dwarf satellite, but cannot directly remove the denser interstellar medium. This suggests that star-formation-driven outflows serve two purposes in quenching satellites in low-mass environments: outflows from the host form a low-density circumgalactic medium that cannot directly strip the interstellar media from its satellites, but is sufficient to remove loosely-bound gaseous outflows from the dwarf satellites driven by their own star formation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09262v1

Spiraling stars in the Small Magellanic Cloud are the subject of a recent study in ‘The Astrophysical Journal.' Find out how their spiral motions help explain the “baby boom” of star formation shortly after the Big Bang. This episode is also available as a blog post: http://daretoknow.ca/2022/09/09/spiraling-stars-help-explain-early-universe/ --- Send in a voice message: https://anchor.fm/david-morton-rintoul/message

The internal line-of-sight kinematics of NGC 346: the rotation of the core region by Peter Zeidler et al. on Thursday 08 September We present the stellar radial velocity analysis of the central 1x1' of the young massive Small Magellanic Cloud star cluster NGC 346. Using VLT/MUSE integral field spectroscopy in combination with Hubble Space Telescope photometry we extract 103 spectra of cluster member stars suited to measure accurate line-of-sight kinematics. The cluster member stars show two distinct velocity groups at v1 = -3.3 (+0.3/-0.2) km/s and v2 = 2.6 (+0.1/-0.1) km/s, relative to the systemic velocity of 165.5+/-0.2 km/s, and hint for a third group at v3 = 9.4 (+0.1/-0.1 km/s. We show that there is neither a correlation between the velocity groups and the spatial location of the stars, nor their locus on optical color-magnitude diagrams, which makes the stellar velocity a key parameter to separate individual stellar components in such a young star cluster. Velocity group 2 shows clear rotation with Omega2 = -0.4 +/- 0.1 1/Myr, corresponding to -4.9+/-0.7 km/s at radial distance of 10 pc from the center, a possible remnant of the formation process of NGC 346 through the hierarchical collapse of the giant molecular cloud. The ionizing gas has lost any natal kinematic imprint and shows clear expansion, driven by far ultra violet fluxes and stellar winds of the numerous OB stars in the cluster center. The size of this expanding bubble and its expansion velocity of 7.9 km/s is in excellent agreement with the estimate that the latest star formation episode occurred about two million years ago. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03237v1

The internal line-of-sight kinematics of NGC 346: the rotation of the core region by Peter Zeidler et al. on Thursday 08 September We present the stellar radial velocity analysis of the central 1x1' of the young massive Small Magellanic Cloud star cluster NGC 346. Using VLT/MUSE integral field spectroscopy in combination with Hubble Space Telescope photometry we extract 103 spectra of cluster member stars suited to measure accurate line-of-sight kinematics. The cluster member stars show two distinct velocity groups at v1 = -3.3 (+0.3/-0.2) km/s and v2 = 2.6 (+0.1/-0.1) km/s, relative to the systemic velocity of 165.5+/-0.2 km/s, and hint for a third group at v3 = 9.4 (+0.1/-0.1 km/s. We show that there is neither a correlation between the velocity groups and the spatial location of the stars, nor their locus on optical color-magnitude diagrams, which makes the stellar velocity a key parameter to separate individual stellar components in such a young star cluster. Velocity group 2 shows clear rotation with Omega2 = -0.4 +/- 0.1 1/Myr, corresponding to -4.9+/-0.7 km/s at radial distance of 10 pc from the center, a possible remnant of the formation process of NGC 346 through the hierarchical collapse of the giant molecular cloud. The ionizing gas has lost any natal kinematic imprint and shows clear expansion, driven by far ultra violet fluxes and stellar winds of the numerous OB stars in the cluster center. The size of this expanding bubble and its expansion velocity of 7.9 km/s is in excellent agreement with the estimate that the latest star formation episode occurred about two million years ago. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03237v1

The internal proper motion kinematics of NGC346: past formation and future evolution by E. Sabbi et al. on Thursday 08 September We investigate the internal kinematics of the young star-forming region NGC 346 in the Small Magellanic Cloud. We used two epochs of deep F555W and F814W Hubble Space Telescope ACS observations with an 11-year baseline to determine proper motions, and study the kinematics of different populations, as identified by their color-magnitude diagram and spatial distribution characteristics. The proper motion field of the young stars shows a complex structure with spatially coherent patterns. NGC 346 upper-main sequence and pre-main sequence stars follow very similar motion patterns, with the outer parts of the cluster being characterized both by outflows and inflows. The proper motion field in the inner ~10 pc shows a combination of rotation and inflow, indicative of inspiraling motion. The rotation velocity in this regions peaks at ~3 km/s, whereas the inflow velocity peaks at ~1 km/s. Sub-clusters and massive young stellar objects in NGC 346 are found at the interface of significant changes in the coherence of the proper motion field. This suggests that turbulence is the main star formation driver in this region. The similar kinematics observed in the metal-poor NGC 346 and the Milky Way star-forming regions suggest that the differences in the cooling conditions due to the different amounts of metallicity and dust density between the SMC and our Galaxy are too small to alter significantly the process of star clusters assembly and growth. The main characteristics of our findings are consistent with various proposed star cluster formation models. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03215v1

The internal proper motion kinematics of NGC346: past formation and future evolution by E. Sabbi et al. on Thursday 08 September We investigate the internal kinematics of the young star-forming region NGC 346 in the Small Magellanic Cloud. We used two epochs of deep F555W and F814W Hubble Space Telescope ACS observations with an 11-year baseline to determine proper motions, and study the kinematics of different populations, as identified by their color-magnitude diagram and spatial distribution characteristics. The proper motion field of the young stars shows a complex structure with spatially coherent patterns. NGC 346 upper-main sequence and pre-main sequence stars follow very similar motion patterns, with the outer parts of the cluster being characterized both by outflows and inflows. The proper motion field in the inner ~10 pc shows a combination of rotation and inflow, indicative of inspiraling motion. The rotation velocity in this regions peaks at ~3 km/s, whereas the inflow velocity peaks at ~1 km/s. Sub-clusters and massive young stellar objects in NGC 346 are found at the interface of significant changes in the coherence of the proper motion field. This suggests that turbulence is the main star formation driver in this region. The similar kinematics observed in the metal-poor NGC 346 and the Milky Way star-forming regions suggest that the differences in the cooling conditions due to the different amounts of metallicity and dust density between the SMC and our Galaxy are too small to alter significantly the process of star clusters assembly and growth. The main characteristics of our findings are consistent with various proposed star cluster formation models. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03215v1

Multiwavelength modeling the SED of Luminous Supersoft X-ray Sources in Large Magellanic Cloud and Small Magellanic Cloud by Augustin Skopal. on Wednesday 07 September Classical supersoft X-ray sources (SSSs) are understood as close binary systems in which a massive white dwarf (WD) accretes from its companion at rates sustaining steady hydrogen burning on its surface generating bolometric luminosities of $10^{36}-2times10^{38}$ erg/s. Here, we perform for the first time the global supersoft X-rays to near-infrared (NIR) spectral energy distribution (SED) for the brightest SSSs in LMC and SMC. We test a model in which the ultraviolet--NIR is dominated by the emission from a compact (unresolved) circumstellar nebula represented by the ionized gas out-flowing from the SSS. The SED models correspond to luminosities of SSSs a few times $10^{38}-10^{39}$ erg/s, radiating at blackbody temperatures of $approx 3times 10^{5}$ K, and indicate nebular continuum, whose emission measure of $gtrsim 2times10^{60}$ cm$^{-3}$ corresponds to a wind mass-loss at rates $gtrsim 2times 10^{-6}$ $M_{odot},{rm yr}^{-1}$. Such extreme parameters suggest that the brightest SSSs could be unidentified optical novae in a post-nova SSS state sustained at a high long-lasting luminosity by resumed accretion, possibly at super-Eddington rates. New observations and theoretical multiwavelength modeling of the global SED of SSSs are needed to reliably determine their parameters, and thus understand their proper stage in stellar evolution. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02524v1

Multiwavelength modeling the SED of Luminous Supersoft X-ray Sources in Large Magellanic Cloud and Small Magellanic Cloud by Augustin Skopal. on Wednesday 07 September Classical supersoft X-ray sources (SSSs) are understood as close binary systems in which a massive white dwarf (WD) accretes from its companion at rates sustaining steady hydrogen burning on its surface generating bolometric luminosities of $10^{36}-2times10^{38}$ erg/s. Here, we perform for the first time the global supersoft X-rays to near-infrared (NIR) spectral energy distribution (SED) for the brightest SSSs in LMC and SMC. We test a model in which the ultraviolet--NIR is dominated by the emission from a compact (unresolved) circumstellar nebula represented by the ionized gas out-flowing from the SSS. The SED models correspond to luminosities of SSSs a few times $10^{38}-10^{39}$ erg/s, radiating at blackbody temperatures of $approx 3times 10^{5}$ K, and indicate nebular continuum, whose emission measure of $gtrsim 2times10^{60}$ cm$^{-3}$ corresponds to a wind mass-loss at rates $gtrsim 2times 10^{-6}$ $M_{odot},{rm yr}^{-1}$. Such extreme parameters suggest that the brightest SSSs could be unidentified optical novae in a post-nova SSS state sustained at a high long-lasting luminosity by resumed accretion, possibly at super-Eddington rates. New observations and theoretical multiwavelength modeling of the global SED of SSSs are needed to reliably determine their parameters, and thus understand their proper stage in stellar evolution. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02524v1

Our heroes travel to the Small Magellanic Cloud. Seeking aid in repelling the Hegemony of Arcjin or at least information on how this small galaxy had repealed them before. This mission seems to have attracted the attention of the Satrap Sk' Aar, Head of the Hegemony's entire military apparatus. Theme by TeknoAXE #actualplay #superheroes #iconsrpg

Learn about why short-term pleasures are important for your well-being; a Thorne-Żytkow Object, which is what astronomers call a star within a star; and how science identified the culprit for your smelly armpits: Staphylococcus hominis. Short-term pleasures contribute to well-being just as much as self-control by Kelsey Donk Hedonism leads to happiness. (2020). EurekAlert! https://www.eurekalert.org/pub_releases/2020-07/uoz-hlt072720.php  Bernecker, K., & Becker, D. (2020). Beyond Self-Control: Mechanisms of Hedonic Goal Pursuit and Its Relevance for Well-Being. Personality and Social Psychology Bulletin, 014616722094199. https://doi.org/10.1177/0146167220941998 A Thorne-Żytkow Object Is a Star Within a Star by Ashley Hamer Levesque, E. M., Massey, P., Żytkow, A. N., & Morrell, N. (2014). Discovery of a Thorne–Żytkow object candidate in the Small Magellanic Cloud. Monthly Notices of the Royal Astronomical Society: Letters, 443(1), L94–L98. https://doi.org/10.1093/mnrasl/slu080  ‌University of Colorado, & Observatory, L. (2014, June 9). The objects are hybrids of red supergiant and neutron stars that superficially resemble normal red supergiants. Astronomy.Com. https://astronomy.com/news/2014/06/astronomers-discover-first-thorne-zytkow-object-a-bizarre-type-of-hybrid-star  Charley, S. (2012, January 13). How to Make an Element. Pbs.org; Nova. https://www.pbs.org/wgbh/nova/article/make-an-element/  Neutron Stars, Pulsars, and Magnetars - Introduction. (2017). Nasa.gov. https://imagine.gsfc.nasa.gov/science/objects/neutron_stars1.html  Scientists have identified the enzyme responsible for smelly armpits by Grant Currin Life in the pits: Scientists identify the key enzyme behind BO. (2020). EurekAlert! https://www.eurekalert.org/pub_releases/2020-07/uoy-lit072420.php  Sample, I. (2020, July 27). Know sweat: scientists solve mystery behind body odour. The Guardian; The Guardian. https://www.theguardian.com/science/2020/jul/27/know-sweat-scientists-solve-mystery-behind-body-odour  ‌Rudden, M., Herman, R., Rose, M., Bawdon, D., Cox, D. S., Dodson, E., Holden, M. T. G., Wilkinson, A. J., James, A. G., & Thomas, G. H. (2020). The molecular basis of thioalcohol production in human body odour. Scientific Reports, 10(1). https://doi.org/10.1038/s41598-020-68860-z  Subscribe to Curiosity Daily to learn something new every day with Cody Gough and Ashley Hamer. You can also listen to our podcast as part of your Alexa Flash Briefing; Amazon smart speakers users, click/tap “enable” here: https://www.amazon.com/Curiosity-com-Curiosity-Daily-from/dp/B07CP17DJY See omnystudio.com/policies/listener for privacy information.

Astrophiz 101: Professor Melanie Johnston-Hollitt - Directing the Murchison Widefield array Our feature interview this month is with Professor Melanie Johnston-Hollitt, Director of the Murchison Widefield Array & Research Professor based in Western Australia. Melanie manages large-scale, multinational research infrastructure, is regularly involved with international science diplomacy, and she regularly gives advice and consultancy for Governments. Her research specialises in Radio Astrophysics, Telescope Design, and Scientific Visualization. You will love hearing about her work using the sky as a big data archive, the cosmic web, chasing the EOR, colliding galaxy clusters and science as a human endeavour! So cool & exciting In a world that’s changing rapidly, we are making a change to our podcast format so you’ll keep getting a fresh Astrophiz every 2 weeks. We are splitting our content so one episode each month will be dedicated to a new guest interview, from the fields of radio astronomy, optical astronomy, space science or particle physics, Also each month you will get to hear from your regular presenter Dr Ian ‘Astroblog' Musgrave, who will preview a sky Guide for you for the coming month, and he will also take you on an astronomical journey of discovery in ‘Ian’s Tangent’. In our next interview-only episode, we talk with Clint Jeffrey, an amateur radio astronomer who works on the technologies for an 8,5metre dish constructed by the radio astronomy section of the astronomical society of Victoria in Australia. The dish is located in a quiet zone in a rural area about 130km north of Melbourne, and they have just achieved ‘First Light’ with a successful observation of the redshift of the Small Magellanic Cloud, and captured the galactic hydrogen inside the Milky Way.

Michael A. Martin: The Red King. Searching for a lost Romulan fleet, Captain Riker and the Titan are swept out of the galaxy along with Commander Donatra and the Valdore. They find themselves in the Small Magellanic Cloud, an area of space visited nearly a century earlier by another Federation starship. An long-sundered offshoot of humanity has claimed this area of space, and when reality itself is threatened by an encroaching anomaly, Riker and his crew must save these lost children of Earth before the entire region is consigned to non-existence. In this episode of Literary Treks, hosts Dan Gunther and Bruce Gibson welcome author Michael A. Martin to the show to discuss Titan: The Red King, which he co-wrote with Andy Mangels. We talk about their experience in launching the Titan series, the origin of the Neyel, Tuvok and Akaar's troubled past, Donatra and the Romulans, religious belief vs. scientific fact, where Titan goes from here, and wrap up with what Michael is working on now and where you can find him online. At the top of the show, we review the latest Star Trek: Waypoint special issue and respond to listener feedback from the Babel Conference for Literary Treks 266: Bringing the Truth Out of the Shadows News Star Trek Waypoint 2019 Comic Review (00:03:46) Listener Feedback (00:26:19) Feature: Michael A. Martin Launching Titan (00:31:32) The Neyel (00:42:49) Tuvok and Akaar (00:53:15) Klingons and Romulans (00:58:42) Religion is Reality (01:05:15) The Sleeper Consequences (01:11:50) Frane Talks to Akaar (01:16:51) Author Collaboration (01:17:51) A New Project and Being a Fan (01:20:48) Final Thoughts (01:24:04) Hosts Dan Gunther and Bruce Gibson Guest Michael A. Martin Production Bruce Gibson (Editor and Producer) Dan Gunther (Producer) C Bryan Jones (Executive Producer) Ken Tripp (Executive Producer) Matthew Rushing (Executive Producer) Richard Marquez (Production Manager) Brandon-Shea Mutala (Patreon Manager) Ken Tripp (Associate Producer) Brandon-Shea Mutala (Associate Producer) Justin Oser (Associate Producer) Norman C. Lao (Associate Producer) Greg Rozier (Associate Producer) Jeffery Harlan (Associate Producer)

Welcome once again to our insanity, this week the professor brings us good news about how the Uncle Sam is allowing the opportunity for online games to be operated by fans when the game is abandoned like a box full of puppies. Can you help give a game a good home? The DJ says Buck is famous with lawyers, what do you think, is he or is he just a legend in his own lunch box? Perhaps he is famous like Kim Kardashian (we apologise to those who aren’t intellectually challenged here) who was attacked by Jon Bon Jovi (who is believe it or not OLDER then Buck) for only having made a porno. Also, the Fallout76 BETA has a bug that deletes the almost 50 gig game forcing a reinstall. Now that could really suck, particularly if your internet is as bad as the DJ’s. We also discuss the classic Runescape appearing in mobile platform for fans to play once more, and it is a hit. Speaking of the DJ, he brings us news about the Avatar sequels that are currently in production. It is looking like a new Rocky Balboa franchise folks. But honestly, will this be a series of beautiful movies that are as pointless as an umbrella in a hurricane like the first movie? Buck brings us a story of a galactic scale drama in the slow tortured death of a galaxy. But we must ask, is this in fact the first recognised example of an interstellar cupcake with the Milky Way being the victim? But let’s take a moment of silence to witness the death of the Small Magellanic Cloud. In games the Professor plays statues, the video game not the kids one, which apparently might be more fun. The DJ is playing Red Dead Redemption 2, and no, has not been drawing disgusting images in the snow. Buck plays Metro 2033 and is shooting Nazis and Commies. We hope you enjoy our insanity as much as we do, it is always better to be crazy in a group then on your own. Until next week stay safe and watch out for the penguins, they are out there.EPISODE NOTES:US Feds allowing hackers to preserve abandoned internet-based games- https://www.tomshardware.com/news/old-online-games-preserved-federal-government,37992.html - https://arstechnica.com/gaming/2018/10/researchers-can-now-legally-restore-abandoned-online-game-servers/ Fallout 76 Big Bad B.E.T.A Bug- https://www.kotaku.com.au/2018/10/fallout-76-bug-accidentally-deletes-entire-50gb-beta/?fbclid=IwAR0MSxLCh8qzRcX6XbZrPbPmHIcDdgzoMbcmxj78ikJitU1QsHZb5yVE-u0 Avatar movie sequel news- https://screenrant.com/avatar-logo-sequels-papyrus-font/- https://screenrant.com/sigourney-weaver-avatar-4-5-filming/Slow death of a galaxy- https://www.csiro.au/en/News/News-releases/2018/Astronomers-witness-slow-death-of-nearby-galaxy Games currently playingProfessor – Statues - https://store.steampowered.com/app/413680/Statues/Buck – Metro 2033 - https://store.steampowered.com/app/286690/Metro_2033_Redux/DJ – Red Dead Redemption 2 - https://www.rockstargames.com/reddeadredemption2/Other topics discussedOld school RuneScape now on Android - https://www.androidpolice.com/2018/10/30/old-school-runescape-officially-available-android-free-play-release/Legal definitions of abandoned - https://en.wikipedia.org/wiki/Abandonware- https://www.digitaltrends.com/gaming/online-games-dmca-exemption/Bioshock the game- https://en.wikipedia.org/wiki/BioShockDune 2- https://en.wikipedia.org/wiki/Dune_IIEve Online’s massive bug- https://www.eveonline.com/article/about-the-boot.ini-issue/Official title for the person who tames the Toruk – Toruk Makto- https://james-camerons-avatar.fandom.com/wiki/Toruk_MaktoGreat Leonopteryxes, known as Toruk by the Na'vi- https://james-camerons-avatar.fandom.com/wiki/Great_LeonopteryxAvatar the movie- https://en.wikipedia.org/wiki/Avatar_(2009_film)Jon Bon Jovi calls out Kim Kardashian- https://metro.co.uk/2018/10/29/bon-jovi-says-kim-kardashian-is-only-famous-for-making-a-porno-in-scathing-attack-8085331/Ferdinand Magellan bio - https://en.wikipedia.org/wiki/Ferdinand_MagellanMagellanic penguins - https://en.wikipedia.org/wiki/Magellanic_penguinMetro 2033 the book- https://en.wikipedia.org/wiki/Metro_2033Metro 2033 author called the Witcher Author an idiot- https://en.ostrog.com/1478Shoutouts92 years since Harry Houdini died - https://en.wikipedia.org/wiki/Harry_HoudiniFamous Birthdays30 Oct 1939 - Leland H. Hartwell, former president and director of the Fred Hutchinson Cancer Research Center in Seattle, Washington and shared the 2001 Nobel Prize in Physiology or Medicine with Paul Nurse and Tim Hunt, for their discoveries of protein molecules that control the division (duplication) of cells, born in Los Angeles, California - https://en.wikipedia.org/wiki/Leland_H._Hartwell30 Oct 1941 - Theodor W. Hänsch, German physicist, received one fourth of the 2005 Nobel Prize in Physics for "contributions to the development of laser-based precision spectroscopy, including the optical frequency comb technique", sharing the prize with John L. Hall and Roy J. Glauber, born in Heidelberg, Germany - https://en.wikipedia.org/wiki/Theodor_W._H%C3%A4nsch 31 Oct 1795 - John Keats, English Romantic poet (Ode to a Grecian Urn), born in London - https://en.wikipedia.org/wiki/John_Keats31 Oct 1860 - Juliette Gordon Low, American activist and founder of the Girl Scouts of America, born in Savannah, Georgia - https://en.wikipedia.org/wiki/Juliette_Gordon_Low31 Oct 1950 - John Candy, Canadian actor and comedian (SCTV, Uncle Buck), born in Newmarket, Ontario - https://en.wikipedia.org/wiki/John_Candy31 Oct 1961 Peter Jackson, New Zealand film director (Lord of the Rings - Academy Award, Best Director, 2003), born in Wellington, New Zealand - https://en.wikipedia.org/wiki/Peter_JacksonEvents of Interest30 Oct 1866 - Jesse James' gang robs bank in Lexington, Missouri ($2000). - https://www.onthisday.com/date/1866/october/3030 Oct 1905 - George Bernard Shaw's "Mrs Warren's Profession" premieres in NYC. - https://www.onthisday.com/date/1905/october/3030 Oct 1918 - British and Ottoman armistice known as Armistice of Mudros treaty signed. - https://en.wikipedia.org/wiki/Armistice_of_Mudros30 Oct 1938 – Orson Welles broadcasts his radio play of H. G. Wells : The War of the Worlds, causing anxiety in some of the audience in the United States. - https://en.wikipedia.org/wiki/The_War_of_the_Worlds_(radio_drama)30 Oct 1940 - Film premiere of "One Night in the Tropics" first film for Abbott and Costello in Paterson, New Jersey. - https://www.onthisday.com/date/1940/october/3030 Oct 1952 - Clarence Birdseye sells first frozen peas. - https://www.onthisday.com/date/1952/october/30Oct 30 1973 - The Bosphorus Bridge in Istanbul, Turkey is completed, connecting the continents of Europe and Asia over the Bosporus for the first time - https://en.wikipedia.org/wiki/Bosphorus_Bridge30 Oct 1974 – The Rumble in the Jungle boxing match between Muhammad Ali and George Foreman takes place in Zaire. - https://en.wikipedia.org/wiki/The_Rumble_in_the_JungleIntroArtist – Goblins from MarsSong Title – Super Mario - Overworld Theme (GFM Trap Remix)Song Link - https://www.youtube.com/watch?v=-GNMe6kF0j0&index=4&list=PLHmTsVREU3Ar1AJWkimkl6Pux3R5PB-QJ Follow us on Facebook - https://www.facebook.com/NerdsAmalgamated/ Email - Nerds.Amalgamated@gmail.com Twitter - https://twitter.com/NAmalgamated Spotify - https://open.spotify.com/show/6Nux69rftdBeeEXwD8GXrS iTunes - https://itunes.apple.com/au/podcast/top-shelf-nerds/id1347661094 RSS - http://www.thatsnotcanonproductions.com/topshelfnerdspodcast?format=rss

Our feature interview is with Kathryn Neugent, who is PhD Astronomy student researching massive stars at the University of Washington in Seattle, research associate at Lowell Observatory in Arizona, discoverer of an amazing runaway Yellow Supergiant in the Small Magellanic Cloud, Photographer, Backpacker, and animal lover pretty much anywhere and everywhere! Follow @KathrynNeugent on Twitter and her blog at http://kathrynneugent.com Find out about massive Wolf-Rayet stars and Kathryn's team's discovery of a new class of WR Stars, and a new mystery for astronomers to grapple with. This is a wonderful example of how great science, while answering one question, will point to new avenues of discovery.  For observers and astrophotographers Dr Ian Musgrave gives us ‘What’s Up Doc’ and he tells us what to look for in our morning and evening skies, what planets, galaxies and nebula to look for and what occultations are happening. In Ian's Tangent, we look at a solar flare likely to eliminate  the possibility of life (as we know it) on exoplanets orbiting our nearest neighbour, Proxima Centauri B. In the news; *ICRAR - Interstellar visitor found in MWA data *Hubble produces image of a star 9 billion light years away, using a combination of gravitational lensing and microlensing.

Feature Guest: Jason Dittmann Just last month, April 2017, astronomers announced the discovery of an extrasolar planet that has the best shot at harbouring life outside our solar system. To find out what makes LHS 1140b so special and what steps are planned to learn more about this potential alien home, today we’re joined at The Star Spot by the discovery team’s leader Dr. Jason Dittmann. Current in Space The famous nearby star Epsilon Eridani harbours a solar system eerily similar to ours, explains Dave. Then Tony shares what we're learning from the clearest image yet taken of the Milky Way's satellite galaxy, the Small Magellanic Cloud. About Our Guest Jason Dittmann is Postdoctoral Fellow at MIT where he is working with a team led by world famous planetary scientist Sara Seager. Dittmann holds one of the four inaugural 51 Pegasi b Postdoctoral Fellowships, which are provided to scientists studying theoretical, observational, and experimental research in planetary astronomy. Dittmann received his PhD from Harvard University and his research interests are in exoplanets and low-mass stars

Astrophiz 22 is out now on Soundcloud or subscribe in iTunes Part II: The Parkes ‘Dish’ interrogates pulsars to expose gravity waves. We interview Operations Scientist John Sarkissian at the CSIRO Parkes Radio Observatory. He explains how the ‘Spider Dipoles’ that make up the Murchison Widefield Array in remote Western Australia contribute to SKA, how Parkes chase down gravity waves and has detected most of the world’s FRBs (fast radio bursts of unknown origin), after being distracted by ‘perytons’ and microwave ovens. And yes, ‘The Dish’ is searching for Extraterrestrial Intelligence in the international SETI ‘Breakthrough Listen’ project. We’re not saying they’re searching for Aliens ….. but Aliens! Dr Nadezhda in Part I of Stellar Evolution explains how the mass of a star determines its evolutionary path, and next week we will look at the Hetsprung-Russell Diagram “What”s Up in the Sky this Week” for Northern Hemisphere observers and astrophotographers, and for Southern Hemisphere Listeners, December is the best time to see the Large Magellanic Cloud and the Small Magellanic Cloud. We also expose Procyon and curse the moon for demolishing the Geminids Meteor Shower In the News: 1. The Spiderweb galaxy 
2. Imaging a Black Hole Event Horizon 
3. ICRAR tells us the Universe is slowly becoming less energetic (Well, who isn’t ;)

We take your questions from our Facebook page, and find some surprisingly deep answers! Yeah, even for the kind of silly ones. Somehow. We just hope we don't change our minds later, and go back in time to undo it, blowing a hole in the universe the size of the Small Magellanic Cloud. Details about the podcast, links to related articles, and supplemental audio/video are available at FamicomDojo.TV: https://famicomdojo.tv/podcast/120 Leave us a voicemail at 608-492-1923, or share your thoughts on Facebook (https://facebook.com/famicomdojo), Instagram (https://instagram.com/famicomdojo), Twitter (@FamicomDojo), or our Famicom Dojo YouTube channel (https://youtube.com/famicomdojo). Vinnk and SeanOrange pixel art by Louis Lloyd-Judson: https://louistrations.co.uk This podcast is brought to you by the Little Podcast Network. Sponsor an episode, or listen to other great shows at http://LittlePodcast.com.

The Small Magellanic Cloud - also known as the SMC - is one of the closest galaxies to the Milky Way.

The Milky Way galaxy has several small satellite galaxies very close to it. One of them is called the Small Magellanic Cloud.

Transcript: The Small Magellanic Cloud is sixty-three kiloparsecs away and about eight kiloparsecs across. It’s an irregular galaxy with a bar-like configuration of blue stars, most of which are a few billion years old. The Small Magellanic Cloud is connected to the Large Magellanic Cloud by a bridge of cold, diffuse hydrogen gas, originally detected by radio astronomers, called the Magellanic Stream. This extends from the Small Magellanic Cloud in an arc that loops behind the south galactic pole and in the other direction reaches down into the plane of the Milky Way. Both Magellanic Clouds are gravitationally bound to the Milky Way, and their orbits take them through the disk of the galaxy. So the Magellanic Stream is a trail of gas drawn out during such a passage about five hundred million years ago.

The aim of this thesis is to assess the effect of the metallicity on the Cepheid Period-Luminosity (PL) relation. The novelty of the approach adopted in this project consists in the homogeneous analysis of a large sample of Cepheids (72) observed in three galaxies (the Milky Way, the Large Magellanic Cloud and the Small Magellanic Cloud), spanning a factor of ten in metallicity. This allows us to explore the effect of the metallicity on the PL relation in a wide range and to study the gas enrichment histories of three different galaxies. To fulfil this goal, firstly, we have selected a sample of Cepheids for which distances and accurate photometry are available in the literature and we have collected high-resolution, high signal-to-noise spectra of these stars, using the highly advanced facilities of the European Southern Observatory in Chile. Secondly, we have directly measured iron and alpha-elements (O, Na, Mg, Al, Si, Ca, Ti) abundances of our sample from these spectra. We have compared our iron abundances with studies on Galactic and Magellanic Cepheids and found a good agreement for the average values and for the individual stars in common. We have then made a broader comparison with results for the Magellanic Clouds from the analysis of F and K non-variable supergiants (they have ages and temperatures similar to Cepheid stars) and of B stars, which are progenitors of Cepheids, and found a good agreement. Cepheids do not show any peculiar differences with these two other population of stars, this indicate that, during this evolutionary stage, there are no changes of the original iron content of the gas from which they were formed. We have then studied the trends of the individual alpha-elements abundance ratios relative to iron as a function of the iron content of our programme star. We can draw some preliminary conclusion considering oxygen, silicon and calcium as the most reliable indicators among the alpha-elements we have analysed. The trends of the abundance ratios of O, Si and Ca are in fairly good agreement with observational studies on Cepheids and on different kinds of stellar populations in the Galaxy and the Magellanic Clouds. The elemental abundances we have determined were used to investigate the effect of metallicity on the PL relation in the V and K bands, in order to check if there is a change of the effect as wavelength increases. We note different behaviours in the two bands. The metallicity has an effect in the V band in the sense that metal-rich Cepheids are fainter than metal-poor ones, while it does not have any effects in the K band. Thus, to safely measure the distances of galaxies, one can use the PL relation in the infrared bands (namely K), so as to minimise the effect of the metallicity. Using the K band has the additional advantage of reducing the effects of the interstellar extinction to the level of other systematic and random errors.

We take a multi-faceted approach to study galaxy populations in the local universe, using the completed Two Degree Field Galaxy Redshift Survey (2dFGRS), the ``Millennium Run'' LCDM N-body simulation, and a semi-analytic model of galaxy formation. Our investigation covers both small and large scale aspects of the galaxy distribution. This work can be broken into three sections, outlined below. Using the 2dFGRS we explore the higher-order clustering properties of local galaxies to quantify both (i) the linear and non-linear bias of the distribution relative to the underlying matter field, and (ii) the nature of hierarchical scaling in the clustering moments of the galaxy distribution. This last point is the expected signature of an initially Gaussian distribution of matter density fluctuations that evolved under the action of gravitational instability. We show in Chapters 2, 3, and 4 that the 2dFGRS higher-order clustering moments are indeed hierarchical, which we measure up to sixth order for galaxies brighter than M_bJ-5log10 h=-17 and which sample the survey volume out to z~0.3. The moments are found to be well described by the negative binomial probability distribution function, and we rule out, at high significance, other models of galaxy clustering, such as the lognormal distribution. This result holds in redshift space on all scales where we obtain a good statistical signal, typically 0.5< R (h^-1 Mpc) < 30 (i.e. from strongly non-linear to quasi-linear regimes). Interestingly, we find that the moments on larger scales can be significantly altered by two massive superclusters present in the 2dFGRS. The skewness of the galaxy distribution is found to have a weak dependence on galaxy luminosity. We show that a simple linear biasing model provides an inadequate description of the higher order results, suggesting that non-linear biasing is present in the clustering moments of the 2dFGRS. The large-scale distribution of structure within the 2dFGRS allows us to study the properties of the galaxy population as a function of local environment. In Chapter 5 we measure the luminosity function of early and late-types galaxies in survey regions ranging from sparse voids to dense clusters to reveal the dominant population in each. Fitting each luminosity function with a Schechter function allows us to quantify how the bright and faint populations transform with changing density contrast. We find that (i) the population in voids is dominated by late types, with a noticeable deficit of intermediate and bright galaxies relative to the mean, and (ii) cluster regions have an excess of very bright early-type galaxies relative to the mean. When directly comparing faint early and late type galaxies in void and cluster regions, the cluster population shows comparable abundances of both types, whereas in voids the late types dominate by almost an order of magnitude. Of interest to many galaxy formation models is our measurement that reveals that the faint-end slope of the overall luminosity function depends at most weakly on density environment. Finally, in Chapter 6, we develop a self-consistent model of galaxy formation and couple this to the Millennium Run LCDM N-body simulation. This simulation represents a significant step forward in both size and resolution, allowing us to follow the the complete evolutionary histories of approximately 20 million galaxies down to luminosities as faint as the Small Magellanic Cloud in a volume comparable to that sampled by the 2dFGRS. In our galaxy formation model we supplement previous treatments of the growth and activity of central black holes with a new model for `radio' feedback from those active galactic nuclei that lie at the centre of a quasistatic X-ray emitting atmosphere in a galaxy group or cluster. With this we can simultaneously explain (i) the low observed mass drop-out rate in cooling flows, (ii) the exponential cut-off at the bright end of the galaxy luminosity function, and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and thus star formation without itself requiring star formation. Matching galaxy formation models with such observations has previously proved quite challenging.