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Effect of gas percentage during minor mergers on the star formation in galaxies 星系中小合并过程中气体百分比对恒星形成的影响
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921322004781
S. N. Hasan, Swetha Thakkalapally, P. Hasan
{"title":"Effect of gas percentage during minor mergers on the star formation in galaxies","authors":"S. N. Hasan, Swetha Thakkalapally, P. Hasan","doi":"10.1017/S1743921322004781","DOIUrl":"https://doi.org/10.1017/S1743921322004781","url":null,"abstract":"Abstract We study the effect of minor mergers on star formation using simulations. We use GADGET4 code which has both collisionless and hydrodynamical particles. Our goal is to establish a relation between gas percentage present in the galaxies and the star formation in the merged galaxy. We use 1:10 minor mergers and we run the isolated simulations with varying gas percentages in the primary galaxy. We observe that the gas particles convert into stars due to the impact of the minor merger. As the gas percentage increases in the primary disk of the galaxy, more number of stars are formed. We also observed that newly formed star particles settle down in the disk of the primary galaxy and increase the thickness of the disk. We also observe that the thickness of the stellar disk containing the old stars also increases due to the impact of the merger.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84507198","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Gas-Star Formation Cycle in Nearby Galaxies 邻近星系中的气体恒星形成周期
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921322003763
H. Pan, E. Schinnerer, A. Hughes, A. Leroy, B. Groves
{"title":"Gas-Star Formation Cycle in Nearby Galaxies","authors":"H. Pan, E. Schinnerer, A. Hughes, A. Leroy, B. Groves","doi":"10.1017/S1743921322003763","DOIUrl":"https://doi.org/10.1017/S1743921322003763","url":null,"abstract":"Abstract Star formation, from cold giant molecular clouds to diverse population of stars, is a complex process involving a wide variety of physical processes. In this work, we constrain the link between the gas-star formation cycle and several secular and environmental probe of galaxies. Specifically, we quantify the spatial correlation between molecular gas and star-forming regions for 49 nearby galaxies using the ALMA and narrowband-Hα imaging from the PHANGS survey. At the resolution (150 pc) at which the individual molecular clouds and star-forming regions can be identified, we find that molecular clouds and star-forming regions do not necessarily coexist. The decoupled molecular clouds and star-forming regions are a signature of evolutionary cycling and feedback of the star formation process. Therefore, the impact of galactic-scale conditions and environments must be considered for a complete understanding of how stars form in galaxies and how this process influences the evolution of the host galaxies.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74430059","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
IAU volume 17 issue 373 Cover and Back matter 国际天文学联合会第17卷第373期封面和封底
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/s1743921323000431
Gómez Medina, H. Golshan
{"title":"IAU volume 17 issue 373 Cover and Back matter","authors":"Gómez Medina, H. Golshan","doi":"10.1017/s1743921323000431","DOIUrl":"https://doi.org/10.1017/s1743921323000431","url":null,"abstract":"","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73476809","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Parsec scale CO depletion in KAGONMA 71, or a star-forming filament in CMa OB1 在KAGONMA 71中秒差距尺度的CO耗尽，或者在CMa OB1中形成恒星的灯丝
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921322004926
T. Handa, Y. Hirata, T. Murase, J. Nishi, Y. Shimajiri, T. Omodaká, M. Nakano, K. Sunada, T. Ito, J. Chibueze
{"title":"Parsec scale CO depletion in KAGONMA 71, or a star-forming filament in CMa OB1","authors":"T. Handa, Y. Hirata, T. Murase, J. Nishi, Y. Shimajiri, T. Omodaká, M. Nakano, K. Sunada, T. Ito, J. Chibueze","doi":"10.1017/S1743921322004926","DOIUrl":"https://doi.org/10.1017/S1743921322004926","url":null,"abstract":"Abstract The depletion of CO molecules is observed in infrared dark clouds. However, only few exsamples are found in pc-scale. An NH3 emission is one of good counter parts of C18O because of similar effective critical density. Our NH3 observations of a molecular filament associated with CMa OB1 or KAG 71, which is a target of Kagoshima Galactic Object survey with Nobeyama 45-m telescope by Mapping in Ammonia lines (KAGONMA) project. Although NH3 data shows similarity in morphology with infrared data suggesting no depletion, C18O in the clumps 4 and 6 are weaker than expected based on NH3 data. After examining the dissipation of the high-density gas, photodissociation, and depletion, we concluded that CO is depleted at least in the clump 4. It is a new example of depletion in pc-scale.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83919017","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
SWAG: The Maps SWAG:地图
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921323000182
J. Ott, David S. Meier, T. Candelaria, D. Ward
{"title":"SWAG: The Maps","authors":"J. Ott, David S. Meier, T. Candelaria, D. Ward","doi":"10.1017/S1743921323000182","DOIUrl":"https://doi.org/10.1017/S1743921323000182","url":null,"abstract":"Abstract We present maps of the “Survey of Water and Ammonia toward the Galactic center” (SWAG). SWAG was observed over three years (∼550 h) with the Australia Telescope Compact Array (ATCA) and covers the entire Central Molecular Zone (CMZ) at about 26” or ∼1 pc resolution. The observed 21.2–25.6 GHz range contains tens of spectral lines and 4 GHz of continuum. Here, we present some final maps. These include multiple NH3 lines, radio recombination lines, shock tracers like HNCO and methanol (CH3OH), high resolution 22 GHz water masers, and a continuum map. The maps are the foundation for ongoing comprehensive temperature mapping of the CMZ, including the identification of heating mechanisms, the characterization of water maser sources as young stellar objects or AGB stars, as well as chemistry, dynamics, and star formation studies of the ISM in this unique environment.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72850476","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations 星系模拟中的反馈模型及其对宇宙流体力学模拟的影响
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921323000133
K. Nagamine
{"title":"Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations","authors":"K. Nagamine","doi":"10.1017/S1743921323000133","DOIUrl":"https://doi.org/10.1017/S1743921323000133","url":null,"abstract":"Abstract Feedback effects by supernovae (SNe) and active galactic nuclei (AGNs) are believed to be essential for galaxy evolution and shaping present-day galaxies, but their exact mechanisms on galactic scales and their impact on CGM/IGM are not well understood yet. In galaxy formation simulations, it is still challenging to resolve sub-parsec scales, and we need to implement subgrid models to account for the physics on small scales. In this article, we summarize some of the efforts to build more physically based feedback models, discuss about pushing the resolution to its limits in galaxy simulations, testing galaxy formation codes under the AGORA code comparison project, and how to probe the impact of feedback using cosmological hydrodynamic simulations via Lyα absorption and CGM/IGM tomography technique. We also discuss our future directions of research in this field and how we make progress by comparing our simulations with observations.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77008368","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","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: structure via live potentials 银河系:通过活电位的结构
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921322004902
Eva Durán-Camacho, A. Duarte-Cabral
{"title":"Milky Way: structure via live potentials","authors":"Eva Durán-Camacho, A. Duarte-Cabral","doi":"10.1017/S1743921322004902","DOIUrl":"https://doi.org/10.1017/S1743921322004902","url":null,"abstract":"Abstract We use the AREPO numerical code to model the structure of a Milky Way like galaxy (MW) via a suite of simulations composed of a stellar disc and bulge, a dark matter halo, and a gaseous disc under isothermal conditions. For each model, we produce longitude velocity (l-v) maps of the gas surface densities to extract the skeletons of the main features (arms, bar), and the contours defining the terminal velocities of the gas. We compare these with observations via a number of diagnostic tools, and select the model that best reproduces the main observed features of the Milky Way.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85970404","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
The Progressive Integral Step Method (PrISM) for Wide Field 3D Spectral Imaging of Nearby Galaxies: an Overview of the TYPHOON Survey 近星系宽视场三维光谱成像的渐进式积分阶跃法(PrISM):台风巡天综述
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S174392132200429X
K. Grasha
{"title":"The Progressive Integral Step Method (PrISM) for Wide Field 3D Spectral Imaging of Nearby Galaxies: an Overview of the TYPHOON Survey","authors":"K. Grasha","doi":"10.1017/S174392132200429X","DOIUrl":"https://doi.org/10.1017/S174392132200429X","url":null,"abstract":"Abstract The TYPHOON program is producing an atlas of spectroscopic data cubes of 44 large-angular-sized galaxies with complete spatial coverage from 3650–9000 Å. This survey provides an unparalleled opportunity to study variations in the interstellar medium (ISM) properties within individual H ii regions across the entire star-forming disks of nearby galaxies. This can provide key insights into the spatial distribution and resolved properties of the ISM to understand how efficiently metals are mixed and redistributed across spirals and dwarf galaxies. In this Proceeding, we present early science results from six nearby spiral galaxies as part of the TYPHOON program from Grasha et al. (2022). We use HIIPhot to identify the H ii regions within the galaxy based on the surface brightness of the Hα emisison line and measure variations of the H ii region oxygen abundance. In this initial work, we find that while the spiral pattern plays a role in organizing the ISM, it alone does not establish the relatively uniform azimuthal variations we observe across all the galaxies. Differences in the metal abundances are more likely driven by the strong correlations with the local physical conditions. We find a strong and positive correlation between the ionization parameter and the local abundances as measured by the relative metallicity offset Δ(O/H), indicating a tight relationship between local physical conditions and their localized enrichment of the ISM. These variations can be explained by a combination of localized, star formation-driven self-enrichment and large-scale mixing-driven dilution due to the passing of spiral density waves.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87638589","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
High [OIII] luminosities from star formation and shocks in z∼6 quasars z ~ 6类星体中恒星形成和激波的高[OIII]光度
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/S1743921322003787
Bomee Lee, R. Chary
{"title":"High [OIII] luminosities from star formation and shocks in z∼6 quasars","authors":"Bomee Lee, R. Chary","doi":"10.1017/S1743921322003787","DOIUrl":"https://doi.org/10.1017/S1743921322003787","url":null,"abstract":"Abstract We use archival WISE and Spitzer photometry to derive optical emission line fluxes for a sample of distant quasars at z∼6. We find evidence for exceptionally high equivalent width [OIII] emission (rest-frame EW∼400Å) similar to that inferred for star-forming galaxies at similar redshifts. The median Hα and Hβ equivalent widths are derived to be ∼400Å and ∼100Å respectively, and are consistent with values seen among quasars in the local Universe, and at z ∼ 2. After accounting for the contribution of photoionization in the broad line regions of quasars, we suggest that the narrow [OIII] emission likely arises from feedback due to massive star-formation in the quasar host. Forthcoming mid-infrared spectroscopy with the James Webb Space Telescope will help constrain the physical conditions in quasar hosts further.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91182330","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
IAU volume 17 issue 370 Cover and Front matter 国际天文学联合会第17卷第370期封面和封面问题
Proceedings of the International Astronomical Union Pub Date : 2021-08-01 DOI: 10.1017/s1743921323001011
A. Vidotto, L. Fossati, J. Vink
{"title":"IAU volume 17 issue 370 Cover and Front matter","authors":"A. Vidotto, L. Fossati, J. Vink","doi":"10.1017/s1743921323001011","DOIUrl":"https://doi.org/10.1017/s1743921323001011","url":null,"abstract":"","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2021-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81834957","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
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