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

Low surface brightness dwarf galaxies and their globular cluster populations around the low-density environment of our closest S0 NGC 3115 距离我们最近的 S0 NGC 3115 低密度环境周围的低表面亮度矮星系及其球状星团群

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-18 DOI: 10.1093/mnras/stae2161

Marco A Canossa-Gosteinski, Ana L Chies-Santos, Cristina Furlanetto, Charles J Bonatto, Rodrigo Flores-Freitas, William Schoenell, Michael A Beasley, Roderik Overzier, Basilio X Santiago, Adriano Pieres, Emílio J B Zanatta, Karla A Alamo-Martinez, Eduardo Balbinot, Anna B A Queiroz, Alan Alves-Brito

{"title":"Low surface brightness dwarf galaxies and their globular cluster populations around the low-density environment of our closest S0 NGC 3115","authors":"Marco A Canossa-Gosteinski, Ana L Chies-Santos, Cristina Furlanetto, Charles J Bonatto, Rodrigo Flores-Freitas, William Schoenell, Michael A Beasley, Roderik Overzier, Basilio X Santiago, Adriano Pieres, Emílio J B Zanatta, Karla A Alamo-Martinez, Eduardo Balbinot, Anna B A Queiroz, Alan Alves-Brito","doi":"10.1093/mnras/stae2161","DOIUrl":"https://doi.org/10.1093/mnras/stae2161","url":null,"abstract":"Understanding faint dwarf galaxies is fundamental to the development of a robust theory of galaxy formation on small scales. Since the discovery of a population of ultra diffuse galaxies (UDGs) rich in globular clusters (GCs) in Coma, an increasing number of studies on low surface brightness dwarf galaxies (LSBds) have been published in recent years. The most massive LSBds have been observed predominantly in groups and clusters, with properties displaying dependence on the environment. In this work, we use deep DECam imaging to systematically identify LSBds and their GC populations around the low-density environment of NGC 3115. We carefully analyse the structure and morphology of 24 candidates, 18 of which are reported for the first time. Most candidates exhibit red colours suggesting a connection between their colour and distance to NGC 3115. We followed up with Gemini GMOS imaging 9 LSBds to properly identify their GC populations. We derive lower limits for the number of GCs associated with each galaxy. Our analysis reveals that they occur around of the same loci of Fornax LSB dwarf GC systems. The relationship between the number of GCs and total mass provides a tool in which, by counting the GCs in these galaxies, we estimate an upper limit for the total mass of these LSB dwarfs, obtaining the mean value of ∼3.3 × 1010 M⊙. Our results align with expectations for dwarf-sized galaxies, particularly regarding the distribution and specific frequency of their GC systems.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"24 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256366","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

Modelling hydrogen-deficient carbon stars in MESA— The effects of total mass and mass ratio 模拟 MESA 中的缺氢碳星--总质量和质量比的影响

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-18 DOI: 10.1093/mnras/stae2149

Courtney L Crawford, Nikita Nikultsev, Geoffrey C Clayton, Patrick Tisserand, Jamie Soon, May G Pedersen

{"title":"Modelling hydrogen-deficient carbon stars in MESA— The effects of total mass and mass ratio","authors":"Courtney L Crawford, Nikita Nikultsev, Geoffrey C Clayton, Patrick Tisserand, Jamie Soon, May G Pedersen","doi":"10.1093/mnras/stae2149","DOIUrl":"https://doi.org/10.1093/mnras/stae2149","url":null,"abstract":"Hydrogen-deficient Carbon (HdC) stars are rare, low-mass, chemically peculiar, supergiant variables believed to be formed by a double white dwarf (DWD) merger, specifically of a Carbon/Oxygen- (CO-) and a Helium-white dwarf (He-WD). They consist of two subclasses– the dust-producing R Coronae Borealis (RCB) variables and their dustless counterparts the dustless HdCs (dLHdCs). Additionally, there is another, slightly cooler set of potentially related carbon stars, the DY Persei type variables which have some, but not conclusive, evidence of Hydrogen-deficiency. Recent works have begun to explore the relationship between these three classes of stars, theorizing that they share an evolutionary pathway (a DWD merger) but come from different binary populations, specifically different total masses (Mtot) and mass ratios (q). In this work, we use the mesa modelling framework that has previously been used to model RCB stars and vary the merger parameters, Mtot and q, to explore how those parameters affect the abundances, temperatures, and luminosities of the resultant post-merger stars. We find that lower Mtot and larger q’s both decrease the luminosity and temperatures of post-merger models to the region of the Hertzsprung-Russell Diagram populated by the dLHdCs. These lower Mtot and larger q models also have smaller oxygen isotopic ratios (16O/18O) which is consistent with recent observations of dLHdCs compared to RCBs. None of the models generated in this work can explain the existence of the DY Persei type variables, however this may arise from the assumed metallicity of the models.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"4 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256368","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

Deep learning the intergalactic medium using lyman-alpha forest at 4 ≤ z ≤ 5 利用 4 ≤ z ≤ 5 的莱曼-阿尔法森林深度学习星系间介质

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-18 DOI: 10.1093/mnras/stae2153

Fahad Nasir, Prakash Gaikwad, Frederick B Davies, James S Bolton, Ewald Puchwein, Sarah E I Bosman

{"title":"Deep learning the intergalactic medium using lyman-alpha forest at 4 ≤ z ≤ 5","authors":"Fahad Nasir, Prakash Gaikwad, Frederick B Davies, James S Bolton, Ewald Puchwein, Sarah E I Bosman","doi":"10.1093/mnras/stae2153","DOIUrl":"https://doi.org/10.1093/mnras/stae2153","url":null,"abstract":"Unveiling the thermal history of the intergalactic medium (IGM) at 4 ≤ z ≤ 5 holds the potential to reveal early onset He ii reionization or lingering thermal fluctuations from H i reionization. We set out to reconstruct the IGM gas properties along simulated Lyman-alpha forest data on pixel-by-pixel basis, employing deep neural networks. Our approach leverages the Sherwood-Relics simulation suite, consisting of diverse thermal histories, to generate mock spectra. Our convolutional and residual networks with likelihood metric predicts the Lyα optical depth-weighted density or temperature for each pixel in the Lyα forest skewer. We find that our network can successfully reproduce IGM conditions with high fidelity across range of instrumental signal-to-noise. These predictions are subsequently translated into the temperature-density plane, facilitating the derivation of reliable constraints on thermal parameters. This allows us to estimate temperature at mean cosmic density, T0 , with one sigma confidence, $delta {rm T_{rm 0}},$≲ 1000K, using only one 20h−1cMpc sightline (Δz ≃ 0.04) with a typical reionization history. Existing studies utilize redshift pathlength comparable to Δz ≃ 4 for similar constraints. We can also provide more stringent constraints on the slope (1σ confidence interval, δγ ≲ 0.1) of the IGM temperature-density relation as compared to other traditional approaches. We test the reconstruction on a single high signal-to-noise observed spectrum (20h−1cMpc segment), and recover thermal parameters consistent with current measurements. This machine learning approach has the potential to provide accurate yet robust measurements of IGM thermal history at the redshifts in question.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"33 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269284","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

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