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9 results on '"Mandelker, N."'

1. JWST/NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc

Author

Vanzella, E., Claeyssens, A., Welch, B., Adamo, A., Coe, D., Diego, J. M., Mahler, G., Khullar, G., Kokorev, V., Oguri, M., Ravindranath, S., Furtak, L. J., Hsiao, T. Yu-Yang, Abdurro'uf, Mandelker, N., Brammer, G., Bradley, L. D., Bradac, M., Conselice, C. J., Dayal, P., Nonino, M., Andrade-Santos, F., Windhorst, R. A., Pirzkal, N., Sharon, K., de Mink, S. E., Fujimoto, S., Zitrin, A., Eldridge, J. J., and Norman, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Star cluster formation in the early universe and their contribution to reionization remains to date largely unconstrained. Here we present JWST/NIRCam imaging of the most highly magnified galaxy known at z ~ 6, the Sunrise arc. We identify six young massive star clusters (YMCs) with measured radii spanning ~ 20 pc down to ~ 1 pc (corrected for lensing magnification), estimated stellar masses of ~ $10^{(6-7)}$ Msun, and with ages 1-30 Myr based on SED fitting to photometry measured in 8 filters extending to rest-frame 7000A. The resulting stellar mass surface densities are higher than 1000 Msun pc$^{-2}$ (up to a few $10^5$ Msun pc$^{-2}$) and their inferred dynamical ages qualify the majority of these systems as gravitationally-bound stellar clusters. The star cluster ages map the progression of star formation along the arc, with to evolved systems (>~ 10 Myr old) followed by very young clusters. The youngest stellar clusters (< 5 Myr) show evidence of prominent Hbeta + [OIII]4959,5007 emission, based on photometry, with equivalent widths larger than 1000 A rest-frame, and are hosted in a 200 pc sized star-forming complex. Such a region dominates the ionizing photon production, with a high efficiency log($\xi_{ion}$ [Hz erg$^{-1}$]) ~ 25.7. A significant fraction of the recently formed stellar mass of the galaxy (> 10-30 %) occurred in these YMCs. We speculate that such sources of ionizing radiation boost the ionizing photon production efficiency which eventually carve ionized channels that might favor the escape of Lyman continuum radiation. The survival of some of the clusters would make them the progenitors of massive and relatively metal-poor globular clusters in the local Universe., Comment: 18 pages, 8 figures, 3 tables. ApJ, Accepted

Published
2022
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2. Stellar Masses of Giant Clumps in CANDELS and Simulated Galaxies Using Machine Learning

Author

Huertas-Company, M., Guo, Y., Ginzburg, O., Lee, C. T., Mandelker, N., Metter, M., Primack, J. R., Dekel, A., Ceverino, D., Faber, S. M., Koo, D. C., Koekemoer, A., Snyder, G., Giavalisco, M., and Zhang, H.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A significant fraction of high redshift star-forming disc galaxies are known to host giant clumps, whose nature and role in galaxy evolution are yet to be understood. In this work we first present a new method based on neural networks to detect clumps in galaxy images. We use this method to detect clumps in the rest-frame optical and UV images of a complete sample of $\sim1500$ star forming galaxies at $1

Published
2020
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3. THE AGORA HIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST

Author

Kim, JH, Agertz, O, Teyssier, R, Butler, MJ, Ceverino, D, Choi, JH, Feldmann, R, Keller, BW, Lupi, A, Quinn, T, Revaz, Y, Wallace, S, Gnedin, NY, Leitner, SN, Shen, S, Smith, BD, Thompson, R, Turk, MJ, Abel, T, Arraki, KS, Benincasa, SM, Chakrabarti, S, Degraf, C, Dekel, A, Goldbaum, NJ, Hopkins, PF, Hummels, CB, Klypin, A, Li, H, Madau, P, Mandelker, N, Mayer, L, Nagamine, K, Nickerson, S, O'Shea, BW, Primack, JR, Roca-Fàbrega, S, Semenov, V, Shimizu, I, Simpson, CM, Todoroki, K, Wadsley, JW, and Wise, JH

Subjects
cosmology: theory, galaxies: evolution, galaxies: formation, galaxies: kinematics and dynamics, ISM: structure, methods: numerical, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

Using an isolated Milky Way-mass galaxy simulation, we compare results from nine state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt-Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly formed stellar clump mass functions show more significant variation (difference by up to a factor of ∼3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low-density region, and between more diffusive and less diffusive schemes in the high-density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes.

Published
2016

4. Ultraviolet Perspectives on Diffuse Gas in the Largest Cosmic Structures

Author

Burchett, J., Butsky, I., Tremmel, M., Bordoloi, R., Bryan, G., Cai, Z., Canning, R., Chen, H., Coil, A., Fielding, D., Fumagalli, M., Johnson, S.D., Khaire, V., Lee, K., Lehner, N., Mandelker, N., O'Meara, J., Muzahid, S., Nelson, D., Oppenheimer, B.D., Postman, M., Peeples, M.S., Quinn, T., Rafelski, M., Ribaudo, J., Rubin, K., Stern, J., Tejos, N., Tonnesen, S., Tripp, T., Wang, Q., Willmer, C.N.A., Zheng, Y., Burchett, J, Butsky, I, Tremmel, M, Bordoloi, R, Bryan, G, Cai, Z, Canning, R, Chen, H, Coil, A, Fielding, D, Fumagalli, M, Johnson, S, Khaire, V, Lee, K, Lehner, N, Mandelker, N, O'Meara, J, Muzahid, S, Nelson, D, Oppenheimer, B, Postman, M, Peeples, M, Quinn, T, Rafelski, M, Ribaudo, J, Rubin, K, Stern, J, Tejos, N, Tonnesen, S, Tripp, T, Wang, Q, Willmer, C, and Zheng, Y

Subjects
UV spectroscopy
Abstract

The past decade has seen an explosion of discoveries and new insights into the diffuse gas within galaxies, galaxy clusters, and the filaments composing the Cosmic Web. A new decade will bring fresh opportunities to further this progress towards developing a comprehensive view of the composition, thermal state, and physical processes of diffuse gas in the Universe. Ultraviolet (UV) spectroscopy, probing diffuse 10^4-10^6 K gas at high spectral resolution, is uniquely poised to (1) witness environmental galaxy quenching processes in action, such as strangulation and tidal- and ram-pressure stripping, (2) directly account for the baryon content of galaxy clusters in the cold-warm (T

Published
2019

5. Ultraviolet Perspectives on Diffuse Gas in the Largest Cosmic Structures

Author

Burchett, J, Butsky, I, Tremmel, M, Bordoloi, R, Bryan, G, Cai, Z, Canning, R, Chen, H, Coil, A, Fielding, D, Fumagalli, M, Johnson, S, Khaire, V, Lee, K, Lehner, N, Mandelker, N, O'Meara, J, Muzahid, S, Nelson, D, Oppenheimer, B, Postman, M, Peeples, M, Quinn, T, Rafelski, M, Ribaudo, J, Rubin, K, Stern, J, Tejos, N, Tonnesen, S, Tripp, T, Wang, Q, Willmer, C, Zheng, Y, Burchett, Joseph, Butsky, Iryna, Tremmel, Michael, Bordoloi, Rongmon, Bryan, Greg, Cai, Zheng, Canning, Rebecca, Chen, Hsiao-Wen, Coil, Alison, Fielding, Drummond, Fumagalli, Michele, Johnson, Sean D., Khaire, Vikram, Lee, Khee-Gan, Lehner, Nicolas, Mandelker, Nir, O'Meara, John, Muzahid, Sowgat, Nelson, Dylan, Oppenheimer, Benjamin D., Postman, Marc, Peeples, Molly S., Quinn, Thomas, Rafelski, Marc, Ribaudo, Joseph, Rubin, Kate, Stern, Jonathan, Tejos, Nicolas, Tonnesen, Stephanie, Tripp, Todd, Wang, Q. Daniel, Willmer, Christopher N. A., Zheng, Yong, Burchett, J, Butsky, I, Tremmel, M, Bordoloi, R, Bryan, G, Cai, Z, Canning, R, Chen, H, Coil, A, Fielding, D, Fumagalli, M, Johnson, S, Khaire, V, Lee, K, Lehner, N, Mandelker, N, O'Meara, J, Muzahid, S, Nelson, D, Oppenheimer, B, Postman, M, Peeples, M, Quinn, T, Rafelski, M, Ribaudo, J, Rubin, K, Stern, J, Tejos, N, Tonnesen, S, Tripp, T, Wang, Q, Willmer, C, Zheng, Y, Burchett, Joseph, Butsky, Iryna, Tremmel, Michael, Bordoloi, Rongmon, Bryan, Greg, Cai, Zheng, Canning, Rebecca, Chen, Hsiao-Wen, Coil, Alison, Fielding, Drummond, Fumagalli, Michele, Johnson, Sean D., Khaire, Vikram, Lee, Khee-Gan, Lehner, Nicolas, Mandelker, Nir, O'Meara, John, Muzahid, Sowgat, Nelson, Dylan, Oppenheimer, Benjamin D., Postman, Marc, Peeples, Molly S., Quinn, Thomas, Rafelski, Marc, Ribaudo, Joseph, Rubin, Kate, Stern, Jonathan, Tejos, Nicolas, Tonnesen, Stephanie, Tripp, Todd, Wang, Q. Daniel, Willmer, Christopher N. A., and Zheng, Yong

Abstract

The past decade has seen an explosion of discoveries and new insights into the diffuse gas within galaxies, galaxy clusters, and the filaments composing the Cosmic Web. A new decade will bring fresh opportunities to further this progress towards developing a comprehensive view of the composition, thermal state, and physical processes of diffuse gas in the Universe. Ultraviolet (UV) spectroscopy, probing diffuse 10^4-10^6 K gas at high spectral resolution, is uniquely poised to (1) witness environmental galaxy quenching processes in action, such as strangulation and tidal- and ram-pressure stripping, (2) directly account for the baryon content of galaxy clusters in the cold-warm (T<10^6 K) gas, (3) determine the phase structure and kinematics of gas participating in the equilibrium-regulating exchange of energy at the cores of galaxy clusters, and (4) map cold streams and filaments of the Cosmic Web that feed galaxies and clusters. With a substantial UV undertaking beyond the Hubble Space Telescope, all of the above would be achievable over the entire epoch of galaxy cluster formation. Such capabilities, coupled with already-planned advancements at other wavelengths, will transform extragalactic astronomy by revealing the dominant formation and growth mechanisms of gaseous halos over the mass spectrum, settling the debate between early- and late-time metal enrichment scenarios, and revealing how the ecosystems in which galaxies reside ultimately facilitate their demise....

Published
2019

6. THE AGORA HIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST

Author

Kim, J, Agertz, O, Teyssier, R, Butler, M, Ceverino, D, Choi, J, Feldmann, R, Keller, B, Lupi, A, Quinn, T, Revaz, Y, Wallace, S, Gnedin, N, Leitner, S, Shen, S, Smith, B, Thompson, R, Turk, M, Abel, T, Arraki, K, Benincasa, S, Chakrabarti, S, Degraf, C, Dekel, A, Goldbaum, N, Hopkins, P, Hummels, C, Klypin, A, Li, H, Madau, P, Mandelker, N, Mayer, L, Nagamine, K, Nickerson, S, O'Shea, B, Primack, J, Roca-Fabrega, S, Semenov, V, Shimizu, I, Simpson, C, Todoroki, K, Wadsley, J, Wise, J, Kim J. -H., Agertz O., Teyssier R., Butler M. J., Ceverino D., Choi J. -H., Feldmann R., Keller B. W., Lupi A., Quinn T., Revaz Y., Wallace S., Gnedin N. Y., Leitner S. N., Shen S., Smith B. D., Thompson R., Turk M. J., Abel T., Arraki K. S., Benincasa S. M., Chakrabarti S., Degraf C., Dekel A., Goldbaum N. J., Hopkins P. F., Hummels C. B., Klypin A., Li H., Madau P., Mandelker N., Mayer L., Nagamine K., Nickerson S., O'Shea B. W., Primack J. R., Roca-Fabrega S., Semenov V., Shimizu I., Simpson C. M., Todoroki K., Wadsley J. W., Wise J. H., Kim, J, Agertz, O, Teyssier, R, Butler, M, Ceverino, D, Choi, J, Feldmann, R, Keller, B, Lupi, A, Quinn, T, Revaz, Y, Wallace, S, Gnedin, N, Leitner, S, Shen, S, Smith, B, Thompson, R, Turk, M, Abel, T, Arraki, K, Benincasa, S, Chakrabarti, S, Degraf, C, Dekel, A, Goldbaum, N, Hopkins, P, Hummels, C, Klypin, A, Li, H, Madau, P, Mandelker, N, Mayer, L, Nagamine, K, Nickerson, S, O'Shea, B, Primack, J, Roca-Fabrega, S, Semenov, V, Shimizu, I, Simpson, C, Todoroki, K, Wadsley, J, Wise, J, Kim J. -H., Agertz O., Teyssier R., Butler M. J., Ceverino D., Choi J. -H., Feldmann R., Keller B. W., Lupi A., Quinn T., Revaz Y., Wallace S., Gnedin N. Y., Leitner S. N., Shen S., Smith B. D., Thompson R., Turk M. J., Abel T., Arraki K. S., Benincasa S. M., Chakrabarti S., Degraf C., Dekel A., Goldbaum N. J., Hopkins P. F., Hummels C. B., Klypin A., Li H., Madau P., Mandelker N., Mayer L., Nagamine K., Nickerson S., O'Shea B. W., Primack J. R., Roca-Fabrega S., Semenov V., Shimizu I., Simpson C. M., Todoroki K., Wadsley J. W., and Wise J. H.

Abstract

Using an isolated Milky Way-mass galaxy simulation, we compare results from nine state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt-Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly formed stellar clump mass functions show more significant variation (difference by up to a factor of ∼3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low-density region, and between more diffusive and less diffusive schemes in the high-density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes.

Published
2016

7. Ultraviolet Perspectives on Diffuse Gas in the Largest Cosmic Structures

Author

Burchett, Butsky, J., Tremmel, I., Bordoloi, M., Bryan, R., Cai, G., Canning, Z., Chen, R., Coil, H., Fielding, A., Fumagalli, D., Johnson, M., Khaire, S. D., Lee, V., Lehner, K., Mandelker, N., Meara, N. O., Sowgat Muzahid, Nelson, S., Oppenheimer, D., Postman, B. D., Peeples, M., Quinn, M. S., Rafelski, T., Ribaudo, M., Rubin, J., Stern, K., Tejos, J., Tonnesen, N., Tripp, S., Wang, T., Willmer, Q., and Zheng, C. N. A.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The past decade has seen an explosion of discoveries and new insights into the diffuse gas within galaxies, galaxy clusters, and the filaments composing the Cosmic Web. A new decade will bring fresh opportunities to further this progress towards developing a comprehensive view of the composition, thermal state, and physical processes of diffuse gas in the Universe. Ultraviolet (UV) spectroscopy, probing diffuse 10^4-10^6 K gas at high spectral resolution, is uniquely poised to (1) witness environmental galaxy quenching processes in action, such as strangulation and tidal- and ram-pressure stripping, (2) directly account for the baryon content of galaxy clusters in the cold-warm (T, White Paper submitted to the Astro2020 Decadal Survey

8. THEAGORAHIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST

Author

Daniel Ceverino, Thomas P. Quinn, Oscar Agertz, Brian W. O'Shea, Ikkoh Shimizu, Ben W. Keller, Vadim A. Semenov, Colin DeGraf, Spencer Clark Wallace, John H. Wise, Joel R. Primack, Alessandro Lupi, Nir Mandelker, Lucio Mayer, Keita Todoroki, Britton D. Smith, Jun-Hwan Choi, Avishai Dekel, Robert Thompson, Samantha M. Benincasa, Philip F. Hopkins, Kentaro Nagamine, Sijing Shen, Robert Feldmann, Cameron Hummels, Nickolay Y. Gnedin, Tom Abel, Kenza S. Arraki, Samuel N. Leitner, Sukanya Chakrabarti, James Wadsley, Michael J. Butler, Santi Roca-Fàbrega, Anatoly Klypin, Romain Teyssier, Christine M. Simpson, Piero Madau, Sarah Nickerson, Nathan J. Goldbaum, Matthew J. Turk, Ji-hoon Kim, Yves Revaz, Hui Li, Kim, J, Agertz, O, Teyssier, R, Butler, M, Ceverino, D, Choi, J, Feldmann, R, Keller, B, Lupi, A, Quinn, T, Revaz, Y, Wallace, S, Gnedin, N, Leitner, S, Shen, S, Smith, B, Thompson, R, Turk, M, Abel, T, Arraki, K, Benincasa, S, Chakrabarti, S, Degraf, C, Dekel, A, Goldbaum, N, Hopkins, P, Hummels, C, Klypin, A, Li, H, Madau, P, Mandelker, N, Mayer, L, Nagamine, K, Nickerson, S, O'Shea, B, Primack, J, Roca-Fabrega, S, Semenov, V, Shimizu, I, Simpson, C, Todoroki, K, Wadsley, J, and Wise, J

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], Radiative cooling, ISM: structure, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, 01 natural sciences, methods: numerical, 010305 fluids & plasmas, Particle and Plasma Physics, kinematics and dynamics [galaxies], 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Nuclear, theory, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Galaxy rotation curve, Physics, theory [cosmology], Star formation, Molecular, numerical [methods], Astronomy and Astrophysics, Scale height, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Distribution function, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, galaxies: kinematics and dynamic, structure [ISM], galaxies: evolution, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Physical Chemistry (incl. Structural)
Abstract

Using an isolated Milky Way-mass galaxy simulation, we compare results from 9 state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt-Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly-formed stellar clump mass functions show more significant variation (difference by up to a factor of ~3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low density region, and between more diffusive and less diffusive schemes in the high density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes., 28 pages, 35 figures, Accepted for publication in the Astrophysical Journal, Image resolution greatly reduced, High-resolution version of this article is available at http://www.jihoonkim.org/agora/AGORA_Paper4_draft.pdf, The first paper of the AGORA Initiative is at http://adsabs.harvard.edu/abs/2014ApJS..210...14K, More information on AGORA is at http://www.AGORAsimulations.org/

Published
2016

9. A cosmic stream of atomic carbon gas connected to a massive radio galaxy at redshift 3.8.

Author

Emonts BHC, Lehnert MD, Yoon I, Mandelker N, Villar-Martín M, Miley GK, De Breuck C, Pérez-Torres MA, Hatch NA, and Guillard P

Abstract

The growth of galaxies in the early Universe is driven by accretion of circum- and intergalactic gas. Simulations have predicted that steady streams of cold gas penetrate the dark matter halos of galaxies and provide the raw material necessary to sustain star formation. We report a filamentary stream of gas that extends for 100 kiloparsecs and connects to the massive radio galaxy 4C 41.17. We detected the stream using submillimeter observations of the 3 P 1 to 3 P 0 emission from the [C i] line of atomic carbon, a tracer of neutral atomic or molecular hydrogen gas. The galaxy contains a central gas reservoir that is fueling a vigorous starburst. Our results show that the raw material for star formation can be present in cosmic streams outside galaxies.

Published
2023
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