11 results
Search Results
2. Galaxy catalogs from the Sage Semi-Analytic Model calibrated on The Three Hundred hydrodynamical simulations: A method to push the limits toward lower mass galaxies in dark matter only clusters simulations.
- Author
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Gómez, Jonathan S., Yepes, G., Muñoz, A. Jiménez, and Cui, W.
- Subjects
GALAXY clusters ,DARK matter ,HYDRODYNAMICS ,STELLAR mass ,PHOTOMETRY - Abstract
The new generation of upcoming deep photometric and spectroscopic surveys will allow us to measure the astrophysical properties of faint galaxies in massive clusters. This would demand to produce simulations of galaxy clusters with better mass resolution than the ones available today if we want to make comparisons between the upcoming observations and predictions of cosmological models. But producing full-physics hydrodynamical simulations of the most massive clusters is not an easy task. This would involve billions of computational elements to reliably resolve low mass galaxies similar to those measured in observations. On the other hand, dark matter only simulations of cluster size halos can be done with much larger mass resolution but at the cost of having to apply a model that populate galaxies within each of the subhalos in these simulations. In this paper we present the results of a new set of dark matter only simulations with different mass resolutions within the The Three Hundred project. We have generated catalogs of galaxies with stellar and luminosity properties by applying the Sage Semi-Analytical Model of galaxy formation. To obtain the catalogs consistent with the results from hydrodynamical simulations, the internal physical parameters of Sage were calibrated with the Particle Swarm Optimization method using a subset of full-physics runs with the same mass resolution than the dark matter only ones. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
3. Correction to: Neutron star mass in dark matter clumps.
- Author
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Deliyergiyev, Maksym, Del Popolo, Antonino, and Le Delliou, Morgan
- Subjects
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STELLAR mass , *NEUTRON stars , *DARK matter , *STELLAR parallax , *GALACTIC center - Abstract
The given text appears to be a correction to a previous paper that examined the relationship between neutron star mass and dark matter accumulation within dark matter clumps. The authors identified an error in their code that resulted in distance measurements being given with respect to the Sun instead of the Galactic center. They corrected the distance values and found that the resulting plots changed, but the results and conclusions remained qualitatively similar. The document includes figures and graphs that illustrate the corrected analysis. [Extracted from the article]
- Published
- 2024
- Full Text
- View/download PDF
4. Neutron star mass in dark matter clumps.
- Author
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Deliyergiyev, Maksym, Popolo, Antonino Del, and Le Delliou, Morgan
- Subjects
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STELLAR mass , *DARK matter , *STELLAR evolution , *STELLAR parallax , *GALAXIES , *NEUTRON stars - Abstract
This paper investigates a hypothesis proposed in previous research relating neutron star (NS) mass and its dark matter (DM) accumulation. As DM accumulates, NS mass decreases, predicting lower NS masses toward the Galactic centre. Due to limited NSs data near the Galactic centre, we examine NSs located within DM clumps. Using the CLUMPY code simulations, we determine the DM clumps distribution, with masses from 10 to 108 M⊙ and scales from 10−3 to 10 kpc. These clumps' DM exhibit a peak at the centre, tapering toward the outskirts, resembling our Galaxy's DM distribution. We analyse these DM clumps' NS mass variations, considering diverse DM particle masses and galaxy types. We find relatively stable NS mass within 0.01 – 5 kpc from the clump centre. This stability supports the initial hypothesis, particularly for NSs located beyond 0.01 kpc from the clump centre, where NS mass reaches a plateau around 0.1 kpc. Nevertheless, NS mass near the clump's periphery reveals spatial dependence: NS position within DM clumps influences its mass in Milky Way-type galaxies. Moreover, this dependence varies with the DM model considered. In summary, our study investigates the proposed link between NS mass and DM accumulation by examining NSs within DM clumps. While NS mass remains stable at certain distances from the clump centre, spatial dependencies arise near the clump's outer regions, contingent on the specific DM model. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
5. EDGE: The direct link between mass growth history and the extended stellar haloes of the faintest dwarf galaxies.
- Author
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Goater, Alex, Read, Justin I, Noël, Noelia E D, Orkney, Matthew D A, Kim, Stacy Y, Rey, Martin P, Andersson, Eric P, Agertz, Oscar, Pontzen, Andrew, Vieliute, Roberta, Kataria, Dhairya, and Jeneway, Kiah
- Subjects
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SPIRAL galaxies , *GALAXY clusters , *MILKY Way , *STELLAR mass , *DWARF galaxies , *GALAXY formation , *DARK matter - Abstract
Ultra-faint dwarf galaxies (UFDs) are commonly found in close proximity to the Milky Way and other massive spiral galaxies. As such, their projected stellar ellipticity and extended light distributions are often thought to owe to tidal forces. In this paper, we study the projected stellar ellipticities and faint stellar outskirts of tidally isolated ultra-faints drawn from the 'Engineering Dwarfs at Galaxy Formation's Edge' (EDGE) cosmological simulation suite. Despite their tidal isolation, our simulated dwarfs exhibit a wide range of projected ellipticities (0.03 < ε < 0.85), with many possessing anisotropic extended stellar haloes that mimic tidal tails, but owe instead to late-time accretion of lower mass companions. Furthermore, we find a strong causal relationship between ellipticity and formation time of a UFD, which is robust to a wide variation in the feedback model. We show that the distribution of projected ellipticities in our suite of simulated EDGE dwarfs matches well with a sample of 19 Local Group dwarf galaxies and a sample of 11 isolated dwarf galaxies. Given ellipticity in EDGE arises from an ex-situ accretion origin, the agreement in shape indicates the ellipticities of some observed dwarfs may also originate from a non-tidal scenario. The orbital parameters of these observed dwarfs further support that they are not currently tidally disrupting. If the baryonic content in these galaxies is still tidally intact, then the same may be true for their dark matter content, making these galaxies in our Local Group pristine laboratories for testing dark matter and galaxy formation models. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
6. MaNGA DynPop – IV. Stacked total density profile of galaxy groups and clusters from combining dynamical models of integral-field stellar kinematics and galaxy–galaxy lensing.
- Author
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Wang, Chunxiang, Li, Ran, Zhu, Kai, Shan, Huanyuan, Xu, Weiwei, Cappellari, Michele, Gao, Liang, Li, Nan, Lu, Shengdong, Mao, Shude, Yao, Ji, and Xie, Yushan
- Subjects
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STELLAR initial mass function , *GALAXY clusters , *DARK matter , *STELLAR mass , *KINEMATICS , *DENSITY - Abstract
We present the measurement of total and stellar/dark matter decomposed mass density profile around a sample of galaxy groups and clusters with dynamical masses derived from integral-field stellar kinematics from the MaNGA survey in Paper I and weak lensing derived from the DECaLS imaging survey. Combining the two data sets enables accurate measurement of the radial density distribution from several kpc to Mpc scales. Intriguingly, we find that the excess surface density derived from stellar kinematics in the inner region cannot be explained by simply adding an NFW dark matter halo extrapolated from lensing measurement at a larger scale to a stellar mass component derived from the NASA-Sloan Atlas (NSA) catalogue. We find that a good fit to both data sets requires a stellar mass normalization about three times higher than that derived from the NSA catalogue, which would require an unrealistically too-heavy initial mass function for stellar mass estimation. If we keep the stellar mass normalization to that of the NSA catalogue but allow a varying inner dark matter density profile, we obtain an asymptotic slope of γgnfw = |$1.82_{-0.25}^{+0.15}$| and γgnfw = |$1.48_{-0.41}^{+0.20}$| for the group bin and the cluster bin, respectively, significantly steeper than the NFW case. We also compare the total mass inner density slopes with those from TNG300 and find that the values from the simulation are lower than the observation by about 2σ level. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
7. Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic Star Formation Rate Density 300 Myr after the Big Bang.
- Author
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Robertson, Brant, Johnson, Benjamin D., Tacchella, Sandro, Eisenstein, Daniel J., Hainline, Kevin, Arribas, Santiago, Baker, William M., Bunker, Andrew J., Carniani, Stefano, Cargile, Phillip A., Carreira, Courtney, Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, D'Eugenio, Francesco, Egami, Eiichi, Hausen, Ryan, Helton, Jakob M., and Jakobsen, Peter
- Subjects
STAR formation ,GALAXIES ,STELLAR mass ,STELLAR luminosity function ,DARK matter ,REDSHIFT ,OPTICAL telescopes - Abstract
We characterize the earliest galaxy population in the JADES Origins Field, the deepest imaging field observed with JWST. We make use of ancillary Hubble Space Telescope optical images (five filters spanning 0.4–0.9 μ m) and novel JWST images with 14 filters spanning 0.8−5 μ m, including seven medium-band filters, and reaching total exposure times of up to 46 hr per filter. We combine all our data at >2.3 μ m to construct an ultradeep image, reaching as deep as ≈31.4 AB mag in the stack and 30.3–31.0 AB mag (5 σ, r = 0.″1 circular aperture) in individual filters. We measure photometric redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts z = 11.5−15. These objects show compact half-light radii of R
1/2 ∼ 50−200 pc, stellar masses of M⋆ ∼ 107 −108 M☉ , and star formation rates ∼ 0.1−1 M☉ yr−1 . Our search finds no candidates at 15 < z < 20, placing upper limits at these redshifts. We develop a forward-modeling approach to infer the properties of the evolving luminosity function without binning in redshift or luminosity that marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the impact of nondetections. We find a z = 12 luminosity function in good agreement with prior results, and that the luminosity function normalization and UV luminosity density decline by a factor of ∼2.5 from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical models for evolution of the dark matter halo mass function. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
8. The Next Generation Virgo Cluster Survey (NGVS). XXVII. The Size and Structure of Globular Cluster Systems and Their Connection to Dark Matter Halos.
- Author
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Lim, Sungsoon, Peng, Eric W., Côté, Patrick, Ferrarese, Laura, Roediger, Joel C., Liu, Chengze, Spengler, Chelsea, Sola, Elisabeth, Duc, Pierre-Alain, Sales, Laura V., Blakeslee, John P., Cuillandre, Jean-Charles, Durrell, Patrick R., Emsellem, Eric, Gwyn, Stephen D. J., Lançon, Ariane, Marleau, Francine R., Mihos, J. Christopher, Müller, Oliver, and Puzia, Thomas H.
- Subjects
GLOBULAR clusters ,VIRGO Cluster ,DARK matter ,DWARF galaxies ,STELLAR mass ,STARS - Abstract
We study the size and structure of globular cluster (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting Sérsic profiles, we investigate the relationship between effective radii of GC systems (R
e,gc ) and galaxy properties. GC systems are 2–4 times more extended than host galaxies across the entire stellar mass range of our sample (108.3 M⊙ < M* < 1011.6 M⊙ ). The relationship between Re,gc and galaxy stellar mass exhibits a characteristic "knee" at a stellar mass of Mp ≃ 1010.8 , similar to the galaxy Re –stellar mass relationship. We present a new characterization of the traditional blue and red GC color subpopulations, describing them with respect to host galaxy (g ′ − i ′) color (Δgi ): GCs with similar colors to their hosts have a "red" Δgi , and those significantly bluer GCs have a "blue" Δgi . The GC populations with red Δgi , even in dwarf galaxies, are twice as extended as the stars, suggesting that formation or survival mechanisms favor the outer regions. We find a tight correlation between Re,gc and the total number of GCs, with intrinsic scatter ≲0.1 dex spanning two and three orders of magnitude in size and number, respectively. This holds for both red and blue subpopulations, albeit with different slopes. Assuming that NGC,Total correlates with M200 , we find that the red GC systems have effective radii of roughly 1%–5% R200 , while the blue GC systems in massive galaxies can have sizes as large as ∼10% R200 . Environmental dependence on Re,gc is also found, with lower-density environments exhibiting more extended GC systems at fixed mass. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
9. Understanding shape and centroid deviations in 39 strong lensing galaxy clusters in various dynamical states.
- Author
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Gassis, Raven, Bayliss, Matthew B., Sharon, Keren, Mahler, Guillaume, Gladders, Michael D., Dahle, Håkon, Florian, Michael K., Rigby, Jane R., McDonald, Michael, Elicker, Lauren, and Owens, M. Riley
- Subjects
GALAXY clusters ,DARK matter ,ASTRONOMICAL observations ,CENTROID ,STELLAR mass - Abstract
Through observational tests of strong lensing galaxy clusters, we can test simulation derived structure predictions that follow from Λ Cold Dark Matter (ΛCDM) cosmology. The shape and centroid deviations between the total matter distribution, stellar matter distributions, and hot intracluster gas distribution serve as an observational test of these theoretical structure predictions. We measure the position angles, ellipticities, and locations/centroids of the brightest cluster galaxy (BCG), intracluster light (ICL). the hot intracluster medium (ICM), and the core lensing mass for a sample of strong lensing galaxy clusters from the SDSS Giant Arcs Survey (SGAS). We utilize HST WFC3/1R imaging data to measure the shapes/centroids of the ICL and BCG distributions and use Chandra ACIS-I X-ray data to measure the shapes/centroids of the ICM. Additionally, we measure the concentration parameter (c) and asymmetry parameter (A) to incorporate cluster dynamical state into our analysis. Using this multicomponent approach, we evaluate the different components in terms of their ability to trace out the DM halo of clusters in various dynamical states. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
10. Leaving No Branches Behind: Predicting Baryonic Properties of Galaxies from Merger Trees.
- Author
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Chuang, Chen-Yu, Jespersen, Christian Kragh, Lin, Yen-Ting, Ho, Shirley, and Genel, Shy
- Subjects
GALAXY mergers ,GALAXY formation ,STELLAR mass ,PROPERTIES of matter ,DARK matter ,STAR formation - Abstract
Galaxies play a key role in our endeavor to understand how structure formation proceeds in the Universe. For any precision study of cosmology or galaxy formation, there is a strong demand for huge sets of realistic mock galaxy catalogs, spanning cosmologically significant volumes. For such a daunting task, methods that can produce a direct mapping between dark matter halos from dark matter-only simulations and galaxies are strongly preferred, as producing mocks from full-fledged hydrodynamical simulations or semi-analytical models is too expensive. Here, we present a graph-neural-network-based model that is able to accurately predict key properties of galaxies such as stellar mass, g − r color, star formation rate, gas mass, stellar metallicity, and gas metallicity, purely from dark matter properties extracted from halos along the full assembly history of the galaxies. Tests based on the TNG300 simulation of the IllustrisTNG project show that our model can recover the baryonic properties of galaxies to high accuracy, over a wide redshift range (z = 0–5), for all galaxies with stellar masses more massive than 10
9 M⊙ and their progenitors, with strong improvements over the state-of-the-art methods. We further show that our method makes substantial strides toward providing an understanding of the implications of the IllustrisTNG galaxy formation model. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
11. Early Structure Formation from Primordial Density Fluctuations with a Blue, Tilted Power Spectrum: High-redshift Galaxies.
- Author
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Hirano, Shingo and Yoshida, Naoki
- Subjects
GALACTIC redshift ,POWER spectra ,LARGE scale structure (Astronomy) ,GALAXY spectra ,STELLAR density (Stellar population) ,STELLAR mass - Abstract
Recent observations by the James Webb Space Telescope (JWST) discovered unexpectedly abundant luminous galaxies at high redshift, posing possibly a severe challenge to popular galaxy formation models. We study early structure formation in a cosmological model with a blue, tilted power spectrum (BTPS) given by P (k) ∝ k m s with m
s > 1 at small length scales. We run a set of cosmological N -body simulations and derive the abundance of dark matter halos and galaxies under simplified assumptions on star formation efficiency. The enhanced small-scale power allows rapid nonlinear structure formation at z > 7, and galaxies with stellar mass exceeding 1010 M⊙ can be formed by z = 9. Because of frequent mergers, the structure of galaxies and galaxy groups appears clumpy. The BTPS model reproduces the observed stellar mass density at z = 7–9, and thus eases the claimed tension between galaxy formation theory and recent JWST observations. The large-scale structure of the present-day Universe is largely unaffected by the modification of the small-scale power spectrum. We conduct a systematic study by varying the slope of the small-scale power spectrum to derive constraints on the BTPS model from a set of observations of high-redshift galaxies. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
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