Monthly Notices of the Royal Astronomical Society最新文献_第3页

Relativistic SZ temperatures and hydrostatic mass bias for massive clusters in the FLAMINGO simulations FLAMINGO 模拟中大质量星团的相对论 SZ 温度和流体静力学质量偏差

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-17 DOI: 10.1093/mnras/stae1991

Scott T Kay, Joey Braspenning, Jens Chluba, John C Helly, Roi Kugel, Matthieu Schaller, Joop Schaye

{"title":"Relativistic SZ temperatures and hydrostatic mass bias for massive clusters in the FLAMINGO simulations","authors":"Scott T Kay, Joey Braspenning, Jens Chluba, John C Helly, Roi Kugel, Matthieu Schaller, Joop Schaye","doi":"10.1093/mnras/stae1991","DOIUrl":"https://doi.org/10.1093/mnras/stae1991","url":null,"abstract":"The relativistic Sunyaev-Zel’dovich (SZ) effect can be used to measure intracluster gas temperatures independently of X-ray spectroscopy. Here, we use the large-volume FLAMINGO simulation suite to determine whether SZ y-weighted temperatures lead to more accurate hydrostatic mass estimates in massive ($M_{rm 500c} gt 7.5times 10^{14}, {rm M}_{odot }$) clusters than when using X-ray spectroscopic-like temperatures. We find this to be the case, on average. The median bias in the SZ mass at redshift zero is $leftlangle b rightrangle equiv 1-leftlangle M_{rm 500c,hse}/M_{rm 500c,true} rightrangle = -0.05 pm 0.01$, over 4 times smaller in magnitude than the X-ray spectroscopic-like case, $leftlangle b rightrangle = 0.22 pm 0.01$. However, the scatter in the SZ bias, $sigma _{b} approx 0.2$, is around 40 per cent larger than for the X-ray case. We show that this difference is strongly affected by clusters with large pressure fluctuations, as expected from shocks in ongoing mergers. Selecting the clusters with the best-fitting generalized NFW pressure profiles, the median SZ bias almost vanishes, $leftlangle b rightrangle = -0.009 pm 0.005$, and the scatter is halved to $sigma _{b} approx 0.1$. We study the origin of the SZ/X-ray difference and find that, at $R_{rm 500c}$ and in the outskirts, SZ weighted gas better reflects the hot, hydrostatic atmosphere than the X-ray weighted gas. The SZ/X-ray temperature ratio increases with radius, a result we find to be insensitive to variations in baryonic physics, cosmology, and numerical resolution.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"109 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256369","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Milky Way and Andromeda analogs from the TNG50 simulation TNG50 模拟中的银河系和仙女座类似物

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-17 DOI: 10.1093/mnras/stae2165

Annalisa Pillepich, Diego Sotillo-Ramos, Rahul Ramesh, Dylan Nelson, Christoph Engler, Vicente Rodriguez-Gomez, Martin Fournier, Martina Donnari, Volker Springel, Lars Hernquist

{"title":"Milky Way and Andromeda analogs from the TNG50 simulation","authors":"Annalisa Pillepich, Diego Sotillo-Ramos, Rahul Ramesh, Dylan Nelson, Christoph Engler, Vicente Rodriguez-Gomez, Martin Fournier, Martina Donnari, Volker Springel, Lars Hernquist","doi":"10.1093/mnras/stae2165","DOIUrl":"https://doi.org/10.1093/mnras/stae2165","url":null,"abstract":"We present the properties of Milky Way- and Andromeda-like (MW/M31-like) galaxies simulated within TNG50, the highest-resolution run of the IllustrisTNG suite of ΛCDM magneto-hydrodynamical simulations. We introduce our fiducial selection for MW/M31 analogs, which we propose for direct usage as well as for reference in future analyses. TNG50 contains 198 MW/M31 analogs, i.e. galaxies with stellar disky morphology, with a stellar mass in the range of $M_* = 10^{10.5 - 11.2}~rm {rm M}_{odot }$, and within a MW-like 500 kpc-scale environment at z = 0. These are resolved with baryonic (dark matter) mass resolution of $8.5times 10^4rm {rm M}_{odot }$ ($4.5times 10^5rm {rm M}_{odot }$) and ∼150 pc of average gas spatial resolution in the star-forming regions. The majority of TNG50 MW/M31 analogs at z = 0 exhibit a bar, 60percnt are star-forming, the sample includes 3 Local Group (LG)-like systems, and a number of galaxies host one or more satellites as massive as e.g. the Magellanic Clouds. Even within such a relatively narrow selection, TNG50 reveals a great diversity in galaxy and halo properties, as well as in past histories. Within the TNG50 sample, it is possible to identify several simulated galaxies whose integral and structural properties are consistent, one or more at a time, with those measured for the Galaxy and Andromeda. With this paper, we document and release a series of broadly applicable data products that build upon the IllustrisTNG public release and aim to facilitate easy access and analysis by public users. These include datacubes across snapshots (0 ≤ z ≤ 7) for each TNG50 MW/M31-like galaxy, and a series of value-added catalogs.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"46 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269286","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

CO spectra of the ISM in the Host Galaxies of the most luminous WISE-selected AGNs WISE 选定的最亮 AGN 宿主星系中 ISM 的 CO 光谱

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-15 DOI: 10.1093/mnras/stae2147

Lee R Martin, Andrew W Blain, Tanio Díaz-Santos, Roberto J Assef, Chao-Wei Tsai, Hyunsung D Jun, Peter R M Eisenhardt, Jingwen Wu, Andrey Vayner, Román Fernández Aranda

{"title":"CO spectra of the ISM in the Host Galaxies of the most luminous WISE-selected AGNs","authors":"Lee R Martin, Andrew W Blain, Tanio Díaz-Santos, Roberto J Assef, Chao-Wei Tsai, Hyunsung D Jun, Peter R M Eisenhardt, Jingwen Wu, Andrey Vayner, Román Fernández Aranda","doi":"10.1093/mnras/stae2147","DOIUrl":"https://doi.org/10.1093/mnras/stae2147","url":null,"abstract":"We present observations of mid-J (J = 4–3 or J = 5–4) carbon monoxide (CO) emission lines and continuum emission from a sample of ten of the most luminous (Lbol ≥ 1014 L$rm odot$) Hot Dust-Obscured Galaxies (Hot DOGs) discovered by the Wide-field Infrared Survey Explorer (WISE) with redshifts up to 4.6. We uncover broad spectral lines (FWHM ≥ 400 km s−1) in these objects, suggesting a turbulent molecular interstellar medium (ISM) may be ubiquitous in Hot DOGs. A halo of molecular gas, extending out to a radius of 5 kpc is observed in W2305–0039, likely supplied by 940 km s−1 molecular outflows. W0831+0140 is plausibly the host of a merger between at least two galaxies, consistent with observations made using ionized gas. These CO(4–3) observations contrast with previous CO(1–0) studies of the same sources: the CO(4–3) to CO(1–0) luminosity ratios exceed 300 in each source, suggesting that the lowest excited states of CO are underluminous. These findings show that the molecular gas in Hot DOGs is consistently turbulent, plausibly a consequence of AGN feedback, triggered by galactic mergers.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"28 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256399","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Using the Simba cosmological simulations to measure the planar relation between stellar specific angular momentum, mass and effective surface brightness 利用辛巴宇宙学模拟测量恒星比角动量、质量和有效表面亮度之间的平面关系

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-15 DOI: 10.1093/mnras/stae2145

E Elson

{"title":"Using the Simba cosmological simulations to measure the planar relation between stellar specific angular momentum, mass and effective surface brightness","authors":"E Elson","doi":"10.1093/mnras/stae2145","DOIUrl":"https://doi.org/10.1093/mnras/stae2145","url":null,"abstract":"Stellar mass and specific angular momentum are two properties of a galaxy that are directly related to its formation history, and hence morphology. In this work, the tight planar relationship between stellar specific angular momentum (j*), mass (M*) and mean effective surface brightness (&lt;μeff &gt;) that was recently constrained using ALFALFA galaxies is measured more accurately using galaxies from the Simba cosmological simulation. The distribution of 179 Simba galaxies in log10j* − log10M* - &lt;μeff &gt; space is shown to be very tightly planar with $j_*propto M_*^{0.694}$ and the distribution of perpendicular distances between the galaxies and the plane being approximately Gaussian with rms = 0.057 dex. The parameterised distribution is used with existing j* and &lt;μeff &gt; measurements of 3 607 ALFALFA galaxies and 84 SPARC galaxies to reliably predict their published stellar masses to within ∼0.1 to 0.2 dex over several decades of stellar mass. Thus, this work presents a new method of easily generating accurate galaxy stellar mass estimates for late-type galaxies and provides a new measurement of the fundamental link between galaxy morphology, mass and angular momentum.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"34 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269287","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Validating full-spectrum fitting with a synthetic integral-field spectroscopic observation of the milky way 用对银河系的合成积分场光谱观测验证全谱拟合效果

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2148

Zixian Wang, Sanjib Sharma, Michael R Hayden, Jesse van de Sande, Joss Bland-Hawthorn, Sam Vaughan, Marie Martig, Francesca Pinna

{"title":"Validating full-spectrum fitting with a synthetic integral-field spectroscopic observation of the milky way","authors":"Zixian Wang, Sanjib Sharma, Michael R Hayden, Jesse van de Sande, Joss Bland-Hawthorn, Sam Vaughan, Marie Martig, Francesca Pinna","doi":"10.1093/mnras/stae2148","DOIUrl":"https://doi.org/10.1093/mnras/stae2148","url":null,"abstract":"Ongoing deep IFS observations of disk galaxies provide opportunities for comparison with the Milky Way (MW) to understand galaxy evolution. However, such comparisons are marred by many challenges such as selection effects, differences in observations and methodology, and proper validation of full-spectrum fitting methods. In this study, we present a novel code GalCraft to address these challenges by generating mock IFS data cubes of the MW using simple stellar population models and a mock MW stellar catalog derived from E-Galaxia. We use the widely adopted full-spectrum fitting code pPXF to investigate the ability to recover kinematics and stellar populations for an edge-on mock MW IFS observation. We confirm that differences in kinematics, mean age, [M/H], and [α/Fe] between thin and thick disks can be distinguished. However, the age distribution is overestimated in the ranges between 2 − 4 and 12 − 14 Gyr compared to the expected values. This is likely due to the age spacing and degeneracy of SSP templates. We find systematic offsets in the recovered kinematics due to insufficient spectral resolution and the variation of line-of-sight velocity distribution with age and [M/H]. With future higher resolution and multi-[α/Fe] SSP templates, GalCraft will be useful to validate key signatures such as [α/Fe]-[M/H] distribution at different R and |z| and potentially infer radial migration and kinematic heating efficiency to study detailed chemodynamical evolution of MW-like galaxies.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"187 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256115","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Vertical Shear Instability with Partially Reflecting Boundary Conditions 部分反射边界条件下的垂直剪切失稳

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2141

Yuzi Wu, Cong Yu, Can Cui

引用次数: 0

True unicorns and false positives: Simulated probabilities of dark massive companions to bright stars 真正的独角兽和假阳性：明亮恒星暗质量伴星的模拟概率

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2146

Andrew M Miller, Alexander P Stephan, David V Martin

{"title":"True unicorns and false positives: Simulated probabilities of dark massive companions to bright stars","authors":"Andrew M Miller, Alexander P Stephan, David V Martin","doi":"10.1093/mnras/stae2146","DOIUrl":"https://doi.org/10.1093/mnras/stae2146","url":null,"abstract":"Many compact objects (black holes and neutron stars) exist in binaries. These binaries are normally discovered through their interactions, either from accretion as an X-ray binary or collisions as a gravitational wave source. However, the majority of compact objects in binaries should be non-interacting. Recently proposed discoveries have used radial velocities of a bright star (main sequence or evolved) that are indicative of a massive but dark companion, which is inferred to be a compact object. Unfortunately, this burgeoning new field has been hindered by false positives, including the “Unicorn” (V723 Mon) which was initially believed to be a red giant/black hole binary before being refuted. In this work, we investigate the evolution of stellar binary populations over time, using the binary evolution code COSMIC to simulate binary populations and determine the probability of a candidate object being either a “true Unicorn” (actual compact objects in binaries) or a false positive. We find that main sequence stars have a higher true Unicorn probability than red giants or naked helium stars (an exposed core of an evolved star), particularly if the companion is more massive and is ≥3 times less luminous than the MS star. We also find that a top-heavy initial mass function raises the true Unicorn probability further, that super-solar metallicity reduces the probability, and that most true Unicorns are found at periods ≤100 days. Finally, we find that a significant fraction of true Unicorns do not evolve into x-ray binaries during the age of the universe.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256401","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

White dwarf eccentricity fluctuation and dissipation by AGB convection 白矮星偏心率波动和 AGB 对流耗散

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2136

Yair Cohen, Sivan Ginzburg, Maya Levy, Tal Bar Shalom, Yoav Siman Tov

{"title":"White dwarf eccentricity fluctuation and dissipation by AGB convection","authors":"Yair Cohen, Sivan Ginzburg, Maya Levy, Tal Bar Shalom, Yoav Siman Tov","doi":"10.1093/mnras/stae2136","DOIUrl":"https://doi.org/10.1093/mnras/stae2136","url":null,"abstract":"Millisecond pulsars with white dwarf companions have typical eccentricities $esim 10^{-6}{!-!}10^{-3}$. The eccentricities of helium white dwarfs are explained well by applying the fluctuation–dissipation theorem to convective eddies in their red giant progenitors. We extend this theory to more massive carbon–oxygen (CO) white dwarfs with asymptotic giant branch (AGB) progenitors. Due to the radiation pressure in AGB stars, the dominant factor in determining the remnant white dwarf’s eccentricity is the critical residual hydrogen envelope mass $m_{rm env}$ required to inflate the star to giant proportions. Using a suite of mesa stellar evolution simulations with $Delta m_{rm c}=10^{-3}, {rm M}_{odot }$ core-mass intervals, we resolved the AGB thermal pulses and found that the critical $m_{rm env}propto m_{rm c}^{-6}$. The resulting eccentricity $esim 3times 10^{-3}$ is almost independent of the remnant CO white dwarf’s mass $m_{rm c}$. Nearly all of the measured eccentricities lie below this robust theoretical limit, indicating that the eccentricity is damped during the common-envelope inspiral that follows the unstable Roche lobe overflow of the AGB star. Specifically, we focused on white dwarfs with median masses $m_{rm c}gt 0.6, {rm M}_{odot }$. These massive white dwarfs begin their inspiral with practically identical orbital periods and eccentricities, eliminating any dependence on the initial conditions. For this sub-sample, we find an empirical relation $epropto P^{3/2}$ between the final period and eccentricity that is much tighter than previous studies – motivating theoretical work on the eccentricity evolution during the common envelope phase. The eccentricities of lower mass CO white dwarfs may be explained by alternative formation channels.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"12 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256404","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Prospect of Precision Cosmology and Testing General Relativity using Binary Black Holes- Galaxies Cross-correlation 利用双黑洞-星系交叉相关性检验广义相对论和精密宇宙学的前景

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2139

Samsuzzaman Afroz, Suvodip Mukherjee

{"title":"Prospect of Precision Cosmology and Testing General Relativity using Binary Black Holes- Galaxies Cross-correlation","authors":"Samsuzzaman Afroz, Suvodip Mukherjee","doi":"10.1093/mnras/stae2139","DOIUrl":"https://doi.org/10.1093/mnras/stae2139","url":null,"abstract":"Modified theories of gravity predict deviations from General Relativity (GR) in the propagation of gravitational waves (GW) across cosmological distances. A key prediction is that the GW luminosity distance will vary with redshift, differing from the electromagnetic (EM) luminosity distance due to varying effective Planck mass. We introduce a model-independent, data-driven approach to explore these deviations using multi-messenger observations of dark standard sirens (Binary Black Holes, BBH). By combining GW luminosity distance measurements from dark sirens with Baryon Acoustic Oscillation (BAO) measurements, BBH redshifts inferred from cross-correlation with spectroscopic or photometric galaxy surveys, and sound horizon measurements from the Cosmic Microwave Background (CMB), we can make a data-driven test of GR (jointly with the Hubble constant) as a function of redshift. Using the multi-messenger technique with the spectroscopic DESI galaxy survey, we achieve precise measurements of deviations in the effective Planck mass variation with redshift. For the Cosmic Explorer and Einstein Telescope (CEET), the best precision is approximately 3.6%, and for LIGO-Virgo-KAGRA (LVK), it is 7.4% at a redshift of $rm {z = 0.425}$. Additionally, we can measure the Hubble constant with a precision of about 1.1% from CEET and 7% from LVK over five years of observation with a 75% duty cycle. We also explore the potential of cross-correlation with photometric galaxy surveys from the Rubin Observatory, extending measurements up to a redshift of $rm {z sim 2.5}$. This approach can reveal potential deviations from models affecting GW propagation using numerous dark standard sirens in synergy with DESI and the Rubin Observatory.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"41 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269289","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The JWST EXCELS survey: too much, too young, too fast? Ultra-massive quiescent galaxies at 3 < z < 5 JWST EXCELS巡天：太多、太年轻、太快？3 < z < 5的超大质量静态星系

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-14 DOI: 10.1093/mnras/stae2092

A C Carnall, F Cullen, R J McLure, D J McLeod, R Begley, C T Donnan, J S Dunlop, A E Shapley, K Rowlands, O Almaini, K Z Arellano-Córdova, L Barrufet, A Cimatti, R S Ellis, N A Grogin, M L Hamadouche, G D Illingworth, A M Koekemoer, H -H Leung, C C Lovell, P G Pérez-González, P Santini, T M Stanton, V Wild

{"title":"The JWST EXCELS survey: too much, too young, too fast? Ultra-massive quiescent galaxies at 3 < z < 5","authors":"A C Carnall, F Cullen, R J McLure, D J McLeod, R Begley, C T Donnan, J S Dunlop, A E Shapley, K Rowlands, O Almaini, K Z Arellano-Córdova, L Barrufet, A Cimatti, R S Ellis, N A Grogin, M L Hamadouche, G D Illingworth, A M Koekemoer, H -H Leung, C C Lovell, P G Pérez-González, P Santini, T M Stanton, V Wild","doi":"10.1093/mnras/stae2092","DOIUrl":"https://doi.org/10.1093/mnras/stae2092","url":null,"abstract":"We report ultra-deep, medium-resolution spectroscopic observations for four quiescent galaxies with log$_{10}(M_*/mathrm{M_odot })gt 11$ at $3 lt z lt 5$. These data were obtained with JWST NIRSpec as part of the Early eXtragalactic Continuum and Emission Line Science (EXCELS) survey, which we introduce in this work. The first two galaxies are newly selected from PRIMER UDS imaging, both at $z=4.62$ and separated by 860 pkpc on the sky, within a larger structure for which we confirm several other members. Both formed at $zsimeq 8-10$. These systems could plausibly merge by the present day to produce a local massive elliptical galaxy. The other two ultra-massive quiescent galaxies are previously known at $z=3.99$ and 3.19, with the latter (ZF-UDS-7329) having been the subject of debate as potentially too old and too massive to be accommodated by the $Lambda$-CDM halo-mass function. Both exhibit high stellar metallicities, and for ZF-UDS-7329 we are able to measure the $alpha -$enhancement, obtaining [Mg/Fe] = $0.42^{+0.19}_{-0.17}$. We finally evaluate whether these four galaxies are consistent with the $Lambda$-CDM halo-mass function using an extreme value statistics approach. We find that the $z=4.62$ objects and the $z=3.19$ object are unlikely within our area under the assumption of standard stellar fractions ($f_*simeq 0.1-0.2$). However, these objects roughly align with the most massive galaxies expected under the assumption of 100 per cent conversion of baryons to stars ($f_*$=1). Our results suggest extreme galaxy formation physics during the first billion years, but no conflict with $Lambda$-CDM cosmology.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"4 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256405","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0