20 results on '"Shipp, Nora"'
Search Results
2. Synthetic Gaia DR3 surveys from the FIRE cosmological simulations of Milky-Way-mass galaxies
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Nguyen, Tri, Ou, Xiaowei, Panithanpaisal, Nondh, Shipp, Nora, Necib, Lina, Sanderson, Robyn, and Wetzel, Andrew
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Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astrophysics - Astrophysics of Galaxies - Abstract
The third data release (DR3) of Gaia has provided a five-fold increase in the number of radial velocity measurements of stars, as well as a stark improvement in parallax and proper motion measurements. To help with studies that seek to test models and interpret Gaia DR3, we present nine Gaia synthetic surveys, based on three solar positions in three Milky-Way-mass galaxies of the Latte suite of the Fire-2 cosmological simulations. These synthetic surveys match the selection function, radial velocity measurements, and photometry of Gaia DR3, adapting the code base Ananke, previously used to match the Gaia DR2 release in Sanderson et al. 2020. The synthetic surveys are publicly available and can be found at http://ananke.hub.yt/. Similarly to the previous release of Ananke, these surveys are based on cosmological simulations and thus able to model non-equilibrium dynamical effects, making them a useful tool in testing and interpreting Gaia DR3., 17 pages, 7 tables, 6 figures
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- 2023
3. Streams on FIRE: Populations of Detectable Stellar Streams in the Milky Way and FIRE.
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Shipp, Nora, Panithanpaisal, Nondh, Necib, Lina, Sanderson, Robyn, Erkal, Denis, Li, Ting S., Santistevan, Isaiah B., Wetzel, Andrew, Cullinane, Lara R., Ji, Alexander P., Koposov, Sergey E., Kuehn, Kyler, Lewis, Geraint F., Pace, Andrew B., Zucker, Daniel B., Bland-Hawthorn, Joss, Cunningham, Emily C., Kim, Stacy Y., Lilleengen, Sophia, and Moreno, Jorge
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MILKY Way , *STELLAR populations , *DISTRIBUTION of stars , *STELLAR mass , *DWARF galaxies - Abstract
We present the first detailed comparison of populations of dwarf galaxy stellar streams in cosmological simulations and the Milky Way. In particular, we compare streams identified around 13 Milky Way analogs in the FIRE-2 simulations to streams observed by the Southern Stellar Stream Spectroscopic Survey (S 5). For an accurate comparison, we produce mock Dark Energy Survey (DES) observations of the FIRE streams and estimate the detectability of their tidal tails and progenitors. The number and stellar mass distributions of detectable stellar streams is consistent between observations and simulations. However, there are discrepancies in the distributions of pericenters and apocenters, with the detectable FIRE streams, on average, forming at larger pericenters (out to >110 kpc) and surviving only at larger apocenters (≳40 kpc) than those observed in the Milky Way. We find that the population of high-stellar-mass dwarf galaxy streams in the Milky Way is incomplete. Interestingly, a large fraction of the FIRE streams would only be detected as intact satellites in DES-like observations, since their tidal tails have too low surface brightness to be detectable. We thus predict a population of yet-undetected tidal tails around Milky Way satellites, as well as a population of fully undetected low-surface-brightness stellar streams, and estimate their detectability with the Rubin Observatory. Finally, we discuss the causes and implications of the discrepancies between the stream populations in FIRE and the Milky Way, and explore future avenues for tests of satellite disruption in cosmological simulations. [ABSTRACT FROM AUTHOR]
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- 2023
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4. S5: Probing the Milky Way and Magellanic Clouds potentials with the 6D map of the Orphan–Chenab stream.
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Koposov, Sergey E, Erkal, Denis, Li, Ting S, Da Costa, Gary S, Cullinane, Lara R, Ji, Alexander P, Kuehn, Kyler, Lewis, Geraint F, Pace, Andrew B, Shipp, Nora, Zucker, Daniel B, Bland-Hawthorn, Joss, Lilleengen, Sophia, Martell, Sarah L, and Collaboration), (S5
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MILKY Way ,MAGELLANIC clouds ,LARGE magellanic cloud ,ANGULAR momentum (Mechanics) ,STREAMING video & television ,GALACTIC halos - Abstract
We present a 6D map of the Orphan–Chenab (OC) stream by combining the data from Southern Stellar Stream Spectroscopic Survey (S
5 ) and Gaia. We reconstruct the proper motion, radial velocity, distance, on-sky track, and stellar density along the stream with spline models. The stream has a total luminosity of MV = −8.2 and metallicity of [Fe/H] = −1.9, similar to classical Milky Way (MW) satellites like Draco. The stream shows drastic changes in its physical width varying from 200 pc to 1 kpc, but a constant line-of-sight velocity dispersion of 5 |$\mathrm{km\, s^{-1}}$|. Despite the large apparent variation in the stellar number density along the stream, the flow rate of stars along the stream is remarkably constant. We model the 6D stream track by a Lagrange-point stripping method with a flexible MW potential in the presence of a moving extended Large Magellanic Cloud (LMC). This allows us to constrain the mass profile of the MW within the distance range 15.6 < r < 55.5 kpc, with the best measured enclosed mass of |$(2.85\pm 0.1)\times 10^{11}\, \mathrm{\, M_\odot }$| within 32.4 kpc. Our stream measurements are highly sensitive to the LMC mass profile with the most precise measurement of its enclosed mass made at 32.8 kpc, |$(7.02\pm 0.9)\times 10^{10}\, {\rm M}_\odot$|. We also detect that the LMC dark matter halo extends to at least 53 kpc. The fitting of the OC stream allows us to constrain the past LMC trajectory and the degree of dynamical friction it experienced. We demonstrate that the stars in the OC stream show large energy and angular momentum spreads caused by LMC perturbation. [ABSTRACT FROM AUTHOR]- Published
- 2023
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5. The effect of the deforming dark matter haloes of the Milky Way and the Large Magellanic Cloud on the Orphan-Chenab stream
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Lilleengen, Sophia, Petersen, Michael S., Erkal, Denis, Peñarrubia, Jorge, Koposov, Sergey E., Li, Ting S., Cullinane, Lara R., Ji, Alexander P., Kuehn, Kyler, Lewis, Geraint F., Mackey, Dougal, Pace, Andrew B., Shipp, Nora, Zucker, Daniel B., Bland-Hawthorn, Joss, and Hilmi, Tariq
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) Magellanic Clouds [(galaxies] ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,halo [Galaxy] ,Astrophysics::Solar and Stellar Astrophysics ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,kinematics and dynamics [Galaxy] ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics ,evolution [Galaxy] ,structure [Galaxy] - Abstract
It has recently been shown that the Large Magellanic Cloud (LMC) has a substantial effect on the Milky Way's stellar halo and stellar streams. Here, we explore how deformations of the Milky Way and LMC's dark matter haloes affect stellar streams, and whether these effects are observable. In particular, we focus on the Orphan-Chenab (OC) stream which passes particularly close to the LMC, and spans a large portion of the Milky Way's halo. We represent the Milky Way--LMC system using basis function expansions that capture their evolution in an $N$-body simulation. We present the properties of this system, such as the evolution of the densities and force fields of each galaxy. The OC stream is evolved in this time-dependent, deforming potential, and we investigate the effects of the various moments of the Milky Way and the LMC. We find that the simulated OC stream is strongly influenced by the deformations of both the Milky Way and the LMC, and that this effect is much larger than current observational errors. In particular, the Milky Way dipole has the biggest impact on the stream, followed by the evolution of the LMC's monopole, and the LMC's quadrupole. Detecting these effects would confirm a key prediction of collisionless, cold dark matter, and would be a powerful test of alternative dark matter and alternative gravity models., 17 pages, 10 figures. Accepted for publication in MNRAS
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- 2022
6. S 5
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Li, Ting S., Ji, Alexander P., Pace, Andrew B., Erkal, Denis, Koposov, Sergey E., Shipp, Nora, Da Costa, Gary S., Cullinane, Lara R., Kuehn, Kyler, Lewis, Geraint F., Mackey, Dougal, Simpson, Jeffrey D., Zucker, Daniel B., Ferguson, Peter S., Martell, Sarah L., Bland-Hawthorn, Joss, Balbinot, Eduardo, Tavangar, Kiyan, Drlica-Wagner, Alex, De Silva, Gayandhi M., Simon, Joshua D., Collaboration, S5, Li, TS [0000-0002-9110-6163], Ji, AP [0000-0002-4863-8842], Pace, AB [0000-0002-6021-8760], Erkal, D [0000-0002-8448-5505], Koposov, SE [0000-0003-2644-135X], Shipp, N [0000-0003-2497-091X], Da Costa, GS [0000-0001-7019-649X], Cullinane, LR [0000-0001-8536-0547], Kuehn, K [0000-0003-0120-0808], Lewis, GF [0000-0003-3081-9319], MacKey, D [0000-0002-6529-8093], Simpson, JD [0000-0002-8165-2507], Zucker, DB [0000-0003-1124-8477], Ferguson, PS [0000-0001-6957-1627], Martell, SL [0000-0002-3430-4163], Bland-Hawthorn, J [0000-0001-7516-4016], Balbinot, E [0000-0002-1322-3153], Tavangar, K [0000-0001-6584-6144], Drlica-Wagner, A [0000-0001-8251-933X], Simon, JD [0000-0002-4733-4994], Apollo - University of Cambridge Repository, and Astronomy
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Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astronomy and Astrophysics ,5109 Space Sciences ,Astrophysics - Astrophysics of Galaxies ,51 Physical Sciences - Abstract
We report the kinematic, orbital, and chemical properties of 12 stellar streams with no evident progenitors, using line-of-sight velocities and metallicities from the Southern Stellar Stream Spectroscopic Survey ($S^5$), proper motions from $Gaia$ EDR3, and distances derived from distance tracers or the literature. This data set provides the largest homogeneously analyzed set of streams with full 6D kinematics and metallicities. All streams have heliocentric distances between ${\sim}10-50$ kpc. The velocity and metallicity dispersions show that half of the stream progenitors were disrupted dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs), hereafter referred to as DG and GC streams. Based on the mean metallicities of the streams and the mass-metallicity relation, the luminosities of the progenitors of the DG streams range between Carina and Ursa Major I ($-9.5\lesssim M_V\lesssim-5.5$). Four of the six GC streams have mean metallicities of [Fe/H]$< -2$, more metal-poor than typical Milky Way (MW) GCs at similar distances. Interestingly, the 300S and Jet GC streams are the only streams on retrograde orbits in our dozen stream sample. Finally, we compare the orbital properties of the streams with known DGs and GCs in the MW, finding several possible associations. Some streams appear to have been accreted with the recently discovered Gaia-Enceladus-Sausage system, and others suggest that GCs were formed in and accreted together with the progenitors of DG streams whose stellar masses are similar to Draco to Carina ($\sim10^5-10^6M_\odot$)., 24 pages, 8 Figures, 2 Tables. Accepted for publication in ApJ
- Published
- 2022
7. Snowmass2021 Cosmic Frontier White Paper: Dark Matter Physics from Halo Measurements
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Bechtol, Keith, Birrer, Simon, Cyr-Racine, Francis-Yan, Schutz, Katelin, Adhikari, Susmita, Amin, Mustafa, Banerjee, Arka, Bird, Simeon, Blinov, Nikita, Boddy, Kimberly K., Boehm, Celine, Bundy, Kevin, Buschmann, Malte, Chakrabarti, Sukanya, Curtin, David, Dai, Liang, Drlica-Wagner, Alex, Dvorkin, Cora, Erickcek, Adrienne L., Gilman, Daniel, Heeba, Saniya, Kim, Stacy, Iršič, Vid, Leauthaud, Alexie, Lovell, Mark, Lukić, Zarija, Mao, Yao-Yuan, Mau, Sidney, Mitridate, Andrea, Mocz, Philip, Muñoz, Julian B., Nadler, Ethan O., Peter, Annika H. G., Price-Whelan, Adrian, Robertson, Andrew, Sabti, Nashwan, Sehgal, Neelima, Shipp, Nora, Simon, Joshua D., Singh, Rajeev, Van Tilburg, Ken, Wechsler, Risa H., Widmark, Axel, and Yu, Hai-Bo
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High Energy Physics - Phenomenology ,High Energy Physics - Phenomenology (hep-ph) ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The non-linear process of cosmic structure formation produces gravitationally bound overdensities of dark matter known as halos. The abundances, density profiles, ellipticities, and spins of these halos can be tied to the underlying fundamental particle physics that governs dark matter at microscopic scales. Thus, macroscopic measurements of dark matter halos offer a unique opportunity to determine the underlying properties of dark matter across the vast landscape of dark matter theories. This white paper summarizes the ongoing rapid development of theoretical and experimental methods, as well as new opportunities, to use dark matter halo measurements as a pillar of dark matter physics., White paper submitted to the Proceedings of the US Community Study on the Future of Particle Physics (Snowmass 2021). 88 pages, 9 figures. Comments welcome
- Published
- 2022
8. effect of the deforming dark matter haloes of the Milky Way and the Large Magellanic Cloud on the Orphan–Chenab stream.
- Author
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Lilleengen, Sophia, Petersen, Michael S, Erkal, Denis, Peñarrubia, Jorge, Koposov, Sergey E, Li, Ting S, Cullinane, Lara R, Ji, Alexander P, Kuehn, Kyler, Lewis, Geraint F, Mackey, Dougal, Pace, Andrew B, Shipp, Nora, Zucker, Daniel B, Bland-Hawthorn, Joss, Hilmi, Tariq, and Collaboration), (S5
- Subjects
LARGE magellanic cloud ,DARK matter ,FORCE density ,GALACTIC halos ,GALACTIC evolution - Abstract
It has recently been shown that the Large Magellanic Cloud (LMC) has a substantial effect on the Milky Way's stellar halo and stellar streams. Here, we explore how deformations of the Milky Way and LMC's dark matter haloes affect stellar streams, and whether these effects are observable. In particular, we focus on the Orphan–Chenab (OC) stream which passes particularly close to the LMC and spans a large portion of the Milky Way's halo. We represent the Milky Way–LMC system using basis function expansions that capture their evolution in an N -body simulation. We present the properties of this system, such as the evolution of the densities and force fields of each galaxy. The OC stream is evolved in this time-dependent, deforming potential, and we investigate the effects of the various moments of the Milky Way and the LMC. We find that the simulated OC stream is strongly influenced by the deformations of both the Milky Way and the LMC and that this effect is much larger than current observational errors. In particular, the Milky Way dipole has the biggest impact on the stream, followed by the evolution of the LMC's monopole, and the LMC's quadrupole. Detecting these effects would confirm a key prediction of collisionless, cold dark matter, and would be a powerful test of alternative dark matter and alternative gravity models. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
9. Broken into Pieces::ATLAS and Aliqa Uma as One Single Stream
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Li, Ting S., Koposov, Sergey E., Erkal, Denis, Ji, Alexander P., Shipp, Nora, Pace, Andrew B., Hilmi, Tariq, Kuehn, Kyler, Lewis, Geraint F., Mackey, Dougal, Simpson, Jeffrey D., Wan, Zhen, Zucker, Daniel B., Bland-Hawthorn, Joss, Cullinane, Lara R., Costa, Gary S. Da, Drlica-Wagner, Alex, Hattori, Kohei, Martell, Sarah L., and Sharma, Sanjib
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astro-ph.GA ,Computer Science::Multimedia ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We present the first spectroscopic measurements of the ATLAS and Aliqa Uma streams from the Southern Stellar Stream Spectroscopic Survey (S5), in combination with the photometric data from the Dark Energy Survey and astrometric data from Gaia. From the coherence of spectroscopic membersin radial velocity and proper motion, we find out that these two systems are extremely likely to be one stream with discontinuity in morphology and density on the sky (the \kink" feature). We refer to this entire stream as the ATLAS-Aliqa Uma stream, or the AAU stream. We perform a comprehensive exploration of the effect of baryonic substructures and find that only an encounter with the Sagittarius dwarf ~ 0:5 Gyr ago can create a feature similar to the observed \kink". In addition, we also identify two gaps in the ATLAS component associated with the broadening in the stream width (the \broadening" feature). These gaps have likely been created by small mass perturbers, such as dark matter halos, as the AAU stream is the most distant cold stream known with severe variations in both the stream surface density and the stream track on the sky. With the stream track, stream distance and kinematic information, we determine the orbit of the AAU stream and find that it has been affected by the Large Magellanic Cloud, resulting in a misalignment between the proper motion and stream track. Together with the Orphan-Chenab Stream, AAU is the second stream pair that has been found to be a single stream separated into two segments by external perturbation.
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- 2021
10. Phased arrays: A strategy to lower the energy threshold for neutrinos
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Wissel Stephanie, Avva Jessica, Bechtol Keith, Chesebro Tyler, Cremonesi Linda, Gupta Anusha, Ludwig Andrew, Messino Wesley, Miki Christian, Nichol Ryan, Oberla Eric, Romero-Wolf Andrew, Saltzberg David, Schlupf Chandler, Shipp Nora, Varner Gary, and Vieregg Abigail
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Physics ,QC1-999 - Abstract
In-ice radio arrays are optimized for detecting the highest energy, cosmogenic neutrinos expected to be produced though cosmic ray interactions with background photons. However, there are two expected populations of high energy neutrinos: the astrophysical flux observed by IceCube (~1 PeV) and the cosmogenic flux (~ 1017 eV or 100 PeV). Typical radio arrays employ a noise-riding trigger, which limits their minimum energy threshold based on the background noise temperature of the ice. Phased radio arrays could lower the energy threshold by combining the signals from several channels before triggering, thereby improving the signal-to-noise at the trigger level. Reducing the energy threshold would allow radio experiments to more efficiently overlap with optical Cherenkov neutrino telescopes as well as for more efficient searches for cosmogenic neutrinos. We discuss the proposed technique and prototypical phased arrays deployed in an anechoic chamber and at Greenland’s Summit Station.
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- 2017
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11. Discovery and Modeling of Milky Way Stellar Streams
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Shipp, Nora
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Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Stellar streams, the tidal remnants of accreted globular clusters and dwarf galaxies, are uniquely powerful tools for studying the Milky Way. In particular, they allow for strong constraints on the local distribution of dark matter, and they provide insight into how our Galaxy has evolved over time. Models of stellar streams enable measurements of the overall shape and mass of the Milky Way’s halo, which is sensitive to dark matter and galaxy formation physics. On smaller scales, stellar streams are one of the most promising methods for detecting the presence of small clumps of dark matter, which will allow for unprecedented constraints on the nature of the dark matter particle. Streams also provide important constraints on the formation of the Milky Way stellar halo and the history of hierarchical structure formation in our Galaxy, as predicted by the standard Lambda Cold Dark Matter (LCDM) cosmological model. These studies require a large, well-observed sample of stellar streams with full 6D position and velocity measurements. Until recently, such a population was unattainable, but with the advent of large surveys, observations of stellar streams have improved significantly in recent years. In this thesis, I present my work on assembling and modeling the first such population of stellar streams in 6D. First, I present the discovery of a large sample of stellar streams in the Dark Energy Survey, which increased the known population of streams by ~50%, as well as the discovery of a unique stellar stream associated with the Palomar 13 globular cluster. I then describe the measurement of the velocities of this new sample of stellar streams via spectroscopic survey and with data from the Gaia satellite, and present results of modeling this population of stellar streams to constrain the distribution of matter in our Galaxy, including the mass of the Milky Way’s largest satellite, the Large Magellanic Cloud. Finally, I conclude and discuss future efforts in the study of near-field cosmology with this population of 6D stellar streams.
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- 2021
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12. Astrobites as a Community-led Model for Education, Science Communication, and Accessibility in Astrophysics
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Khullar, Gourav, Kohler, Susanna, Konchady, Tarini, Foley, Mike, Hornsby, Amber L, Reyes, Mithi A de los, Chisari, Nora Elisa, Villar, V Ashley, Shin, Kaitlyn, Doughty, Caitlin, Shipp, Nora, Ramasawmy, Joanna, Penoyre, Zephyr, Lichtenberg, Tim, Storey-Fisher, Kate, Hall, Oliver, Lewis, Briley, Pearlman, Aaron B, Cárdenas-Avendaño, Alejandro, Bridge, Joanna S, González-Egea, Elena, Panwar, Vatsal, Slepian, Zachary, and Zimmerman, Mara
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Physics Education (physics.ed-ph) ,physics.ed-ph ,Physics - Physics Education ,FOS: Physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,astro-ph.IM - Abstract
Support for early career astronomers who are just beginning to explore astronomy research is imperative to increase retention of diverse practitioners in the field. Since 2010, Astrobites has played an instrumental role in engaging members of the community -- particularly undergraduate and graduate students -- in research. In this white paper, the Astrobites collaboration outlines our multi-faceted online education platform that both eases the transition into astronomy research and promotes inclusive professional development opportunities. We additionally offer recommendations for how the astronomy community can reduce barriers to entry to astronomy research in the coming decade., 14 pages, 5 figures (including cover page and list of endorsers); Submitted as an Astro2020 Decadal Survey State of the Profession White Paper. Access the Astrobites in the Classroom lesson plans here: https://tinyurl.com/y6kfszbn
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- 2019
13. Dark Matter Science in the Era of LSST
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Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N., Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K., Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M., Buckley, Matthew R., Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R., Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert Ac, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, William A., Macorra, Axel La, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D., Ferreira, Pedro G., Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Maurizio Giannotti, Gill, Mandeep Ss, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A., González-Morales, Alma X., Grin, Daniel, Gruen, Daniel, Hearin, Andrew P., Hendel, David, Hezaveh, Yashar D., Hirata, Christopher M., Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M. James, Jeltema, Tesla E., Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E., Keeton, Charles R., Khatri, Rishi, Koposov, Sergey E., Koushiappas, Savvas M., Kovetz, Ely D., Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S., Liguori, Michele, Lin, Tongyan, Lisanti, Mariangela, Loverde, Marilena, Lu, Jessica R., Mandelbaum, Rachel, Mao, Yao-Yuan, Mcdermott, Samuel D., Mcnanna, Mitch, Medford, Michael, Meerburg, P. Daniel, Meyer, Manuel, Mirbabayi, Mehrdad, Mishra-Sharma, Siddharth, Marc, Moniez, More, Surhud, Moustakas, John, Muñoz, Julian B., Murgia, Simona, Myers, Adam D., Nadler, Ethan O., Necib, Lina, Newburgh, Laura, Newman, Jeffrey A., Nord, Brian, Nourbakhsh, Erfan, Nuss, Eric, O Connor, Paul, Pace, Andrew B., Padmanabhan, Hamsa, Palmese, Antonella, Peiris, Hiranya V., Peter, Annika Hg, Piacentni, Francesco, Piacentini, Francesco, Plazas, Andrés, Polin, Daniel A., Prakash, Abhishek, Prescod-Weinstein, Chanda, Read, Justin I., Ritz, Steven, Robertson, Brant E., Rose, Benjamin, Rosenfeld, Rogerio, Rossi, Graziano, Samushia, Lado, Sánchez, Javier, Sánchez-Conde, Miguel A., Schaan, Emmanuel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Shipp, Nora, Simon, Joshua D., Simon, Sara, Slatyer, Tracy R., Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Straniero, Oscar, Strigari, Louis E., Tait, Tim Mp, Tollerud, Erik, Troxel, Ma, Tyson, J. Anthony, Uhlemann, Cora, Urenña-López, L. Arturo, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W., Wang, Mei-Yu, Watson, Scott, Wechsler, Risa H., Wittman, David, Xu, Weishuang, Yanny, Brian, Young, Sam, Yu, Hai-Bo, Zaharijas, Gabrijela, Zentner, Andrew R., Zuntz, Joe, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE
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Astrophysics and Astronomy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex] ,Dark matter ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Compact star ,01 natural sciences ,Standard Model ,High Energy Physics - Experiment ,High Energy Physics - Experiment (hep-ex) ,Particle mass ,0103 physical sciences ,[PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex] ,010303 astronomy & astrophysics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,astro-ph.HE ,Physics ,hep-ex ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,13. Climate action ,Fundamental physics ,astro-ph.CO ,[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - High Energy Astrophysical Phenomena ,Particle Physics - Experiment ,dark matter: parameter space ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Astrophysical observations currently provide the only robust, empirical measurements of dark matter. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter., 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io
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- 2019
14. Probing the Fundamental Nature of Dark Matter with the Large Synoptic Survey Telescope
- Author
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Drlica-Wagner, Alex, Mao, Yao-Yuan, Adhikari, Susmita, Armstrong, Robert, Banerjee, Arka, Banik, Nilanjan, Bechtol, Keith, Bird, Simeon, Boddy, Kimberly K, Bonaca, Ana, Bovy, Jo, Buckley, Matthew R, Bulbul, Esra, Chang, Chihway, Chapline, George, Cohen-Tanugi, Johann, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, Dawson, William A, Rivero, Ana Díaz, Dvorkin, Cora, Erkal, Denis, Fassnacht, Christopher D, García-Bellido, Juan, Giannotti, Maurizio, Gluscevic, Vera, Golovich, Nathan, Hendel, David, Hezaveh, Yashar D, Horiuchi, Shunsaku, Jee, M James, Kaplinghat, Manoj, Keeton, Charles R, Koposov, Sergey E, Li, Ting S, Mandelbaum, Rachel, McDermott, Samuel D, McNanna, Mitch, Medford, Michael, Meyer, Manuel, Marc, Moniez, Murgia, Simona, Nadler, Ethan O, Necib, Lina, Nuss, Eric, Pace, Andrew B, Peter, Annika HG, Polin, Daniel A, Prescod-Weinstein, Chanda, Read, Justin I, Rosenfeld, Rogerio, Shipp, Nora, Simon, Joshua D, Slatyer, Tracy R, Straniero, Oscar, Strigari, Louis E, Tollerud, Erik, Tyson, J Anthony, Wang, Mei-Yu, Wechsler, Risa H, Wittman, David, Yu, Hai-Bo, Zaharijas, Gabrijela, Ali-Haïmoud, Yacine, Annis, James, Birrer, Simon, Biswas, Rahul, Blazek, Jonathan, Brooks, Alyson M, Buckley-Geer, Elizabeth, Caputo, Regina, Charles, Eric, Digel, Seth, Dodelson, Scott, Flaugher, Brenna, Frieman, Joshua, Gawiser, Eric, Hearin, Andrew P, Hložek, Renee, Jain, Bhuvnesh, Jeltema, Tesla E, Koushiappas, Savvas M, Lisanti, Mariangela, LoVerde, Marilena, Mishra-Sharma, Siddharth, Newman, Jeffrey A, Nord, Brian, Nourbakhsh, Erfan, Ritz, Steven, Robertson, Brant E, Sánchez-Conde, Miguel A, Slosar, Anže, Tait, Tim MP, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W, Yanny, Brian, and Zentner, Andrew R
- Subjects
astro-ph.HE ,hep-ex ,astro-ph.GA ,Astrophysics::Instrumentation and Methods for Astrophysics ,astro-ph.CO ,hep-ph ,Astrophysics::Cosmology and Extragalactic Astrophysics - Abstract
Astrophysical and cosmological observations currently provide the only robust, empirical measurements of dark matter. Future observations with Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. This white paper represents a community effort to summarize the science case for studying the fundamental physics of dark matter with LSST. We discuss how LSST will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational couplings to the Standard Model, and compact object abundances. Additionally, we discuss the ways that LSST will complement other experiments to strengthen our understanding of the fundamental characteristics of dark matter. More information on the LSST dark matter effort can be found at https://lsstdarkmatter.github.io/ .
- Published
- 2019
15. S5: The Destruction of a Bright Dwarf Galaxy as Revealed by the Chemistry of the Indus Stellar Stream.
- Author
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Hansen, Terese T., Ji, Alexander P., Da Costa, Gary S., Li, Ting S., Casey, Andrew R., Pace, Andrew B., Cullinane, Lara R., Erkal, Denis, Koposov, Sergey E., Kuehn, Kyler, Lewis, Geraint F., Mackey, Dougal, Simpson, Jeffrey D., Shipp, Nora, Zucker, Daniel B., Bland-Hawthorn, Joss, and tion
- Subjects
GLOBULAR clusters ,DWARF galaxies ,ANALYTICAL chemistry - Abstract
The recently discovered Indus stellar stream exhibits a diverse chemical signature compared to what is found for most other streams due to the abundances of two outlier stars, Indus_0 and Indus_13. Indus_13 exhibits an extreme enhancement in rapid neutron-capture (r-)process elements with [Eu/Fe] = + 1.81. It thus provides direct evidence of the accreted nature of r-process-enhanced stars. In this paper we present a detailed chemical analysis of the neutron-capture elements in Indus_13, revealing the star to be slightly actinide poor. The other outlier, Indus_0, displays a globular cluster-like signature with high N, Na, and Al abundances, while the rest of the Indus stars show abundances compatible with a dwarf galaxy origin. Hence, Indus_0 provides the first chemical evidence of a fully disrupted dwarf containing a globular cluster. We use the chemical signature of the Indus stars to discuss the nature of the stream progenitor which was likely a chemically evolved system, with a mass somewhere in the range from Ursa Minor to Fornax. [ABSTRACT FROM AUTHOR]
- Published
- 2021
- Full Text
- View/download PDF
16. Broken into Pieces: ATLAS and Aliqa Uma as One Single Stream.
- Author
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Li, Ting S., Koposov, Sergey E., Erkal, Denis, Ji, Alexander P., Shipp, Nora, Pace, Andrew B., Hilmi, Tariq, Kuehn, Kyler, Lewis, Geraint F., Mackey, Dougal, Simpson, Jeffrey D., Wan, Zhen, Zucker, Daniel B., Bland-Hawthorn, Joss, Cullinane, Lara R., Da Costa, Gary S., Drlica-Wagner, Alex, Hattori, Kohei, Martell, Sarah L., and Sharma, Sanjib
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LARGE magellanic cloud ,ASTROMETRY ,DARK energy ,DARK matter ,GALAXY formation - Abstract
We present the first spectroscopic measurements of the ATLAS and Aliqa Uma streams from the Southern Stellar Stream Spectroscopic Survey (S
5 ), in combination with the photometric data from the Dark Energy Survey and astrometric data from Gaia. From the coherence of spectroscopic members in radial velocity and proper motion, we find that these two systems are extremely likely to be one stream with discontinuity in morphology and density on the sky (the "kink" feature). We refer to this entire stream as the ATLAS-Aliqa Uma stream, or the AAU stream. We perform a comprehensive exploration of the effect of baryonic substructures and find that only an encounter with the Sagittarius dwarf ∼0.5 Gyr ago can create a feature similar to the observed "kink." In addition, we also identify two gaps in the ATLAS component associated with the broadening in the stream width (the "broadening" feature). These gaps have likely been created by small mass perturbers, such as dark matter halos, as the AAU stream is the most distant cold stream known with severe variations in both the stream surface density and the stream track on the sky. With the stream track, stream distance, and kinematic information, we determine the orbit of the AAU stream and find that it has been affected by the Large Magellanic Cloud, resulting in a misalignment between the proper motion and stream track. Together with the Orphan-Chenab Stream, AAU is the second stream pair that has been found to be a single stream separated into two segments by external perturbation. [ABSTRACT FROM AUTHOR]- Published
- 2021
- Full Text
- View/download PDF
17. Stellar streams discovered in the Dark Energy Survey
- Author
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Shipp, Nora, Santiago, Basilio Xavier, and DES Collaboration
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Galaxy ,Via láctea ,Populacoes estelares ,Halo – galaxy ,Matéria escura ,Structure – local group ,Halos - Abstract
We perform a search for stellar streams around the Milky Way using the first 3 yr of multiband optical imaging data from the Dark Energy Survey (DES). We use DES data covering ∼5000 deg2 to a depth of g>23.5 with a relative photometric calibration uncertainty of
- Published
- 2018
18. Discovery of Extended Tidal Tails around the Globular Cluster Palomar 13.
- Author
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Shipp, Nora, Price-Whelan, Adrian M., Tavangar, Kiyan, Mateu, Cecilia, and Drlica-Wagner, Alex
- Published
- 2020
- Full Text
- View/download PDF
19. The Southern Stellar Stream Spectroscopic Survey (S5): Chemical Abundances of Seven Stellar Streams.
- Author
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Ji, Alexander P., Li, Ting S., Hansen, Terese T., Casey, Andrew R., Koposov, Sergey E., Pace, Andrew B., Mackey, Dougal, Lewis, Geraint F., Simpson, Jeffrey D., Bland-Hawthorn, Joss, Cullinane, Lara R., Da Costa, Gary. S., Hattori, Kohei, Martell, Sarah L., Kuehn, Kyler, Erkal, Denis, Shipp, Nora, Wan, Zhen, and Zucker, Daniel B.
- Published
- 2020
- Full Text
- View/download PDF
20. Discovery of a nearby 1700 km s−1 star ejected from the Milky Way by Sgr A.
- Author
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Koposov, Sergey E, Boubert, Douglas, Li, Ting S, Erkal, Denis, Da Costa, Gary S, Zucker, Daniel B, Ji, Alexander P, Kuehn, Kyler, Lewis, Geraint F, Mackey, Dougal, Simpson, Jeffrey D, Shipp, Nora, Wan, Zhen, Belokurov, Vasily, Bland-Hawthorn, Joss, Martell, Sarah L, Nordlander, Thomas, Pace, Andrew B, De Silva, Gayandhi M, and Wang, Mei-Yu
- Subjects
MILKY Way ,STELLAR parallax ,MAIN sequence (Astronomy) ,STELLAR orbits ,STELLAR dynamics - Abstract
We present the serendipitous discovery of the fastest main-sequence hyper-velocity star (HVS) by the Southern Stellar Stream Spectroscopic Survey (S
5 ). The star S5-HVS1 is a ∼2.35 M⊙ A-type star located at a distance of ∼9 kpc from the Sun and has a heliocentric radial velocity of 1017 ± 2.7 |$\mathrm{\, km\, s^{-1}}$| without any signature of velocity variability. The current 3D velocity of the star in the Galactic frame is 1755 ± 50 |$\mathrm{\, km\, s^{-1}}$|. When integrated backwards in time, the orbit of the star points unambiguously to the Galactic Centre, implying that S5-HVS1 was kicked away from Sgr A* with a velocity of ∼1800 |$\mathrm{\, km\, s^{-1}}$| and travelled for 4.8 Myr to its current location. This is so far the only HVS confidently associated with the Galactic Centre. S5-HVS1 is also the first hyper-velocity star to provide constraints on the geometry and kinematics of the Galaxy, such as the Solar motion Vy ,⊙ = 246.1 ± 5.3 |$\mathrm{\, km\, s^{-1}}$| or position R0 = 8.12 ± 0.23 kpc. The ejection trajectory and transit time of S5-HVS1 coincide with the orbital plane and age of the annular disc of young stars at the Galactic Centre, and thus may be linked to its formation. With the S5-HVS1 ejection velocity being almost twice the velocity of other hyper-velocity stars previously associated with the Galactic Centre, we question whether they have been generated by the same mechanism or whether the ejection velocity distribution has been constant over time. [ABSTRACT FROM AUTHOR]- Published
- 2020
- Full Text
- View/download PDF
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