Galactic anatomy : the warp, bar, and spin of disk galaxies

다국어 초록 (Multilingual Abstract)

Warps and bars represent prominent morphological characteristics found within both the outer regions and central regions of our Milky Way, and these features are widespread in nearby disk galaxies. Consequently, it becomes imperative to gain a comprehensive understanding of how these structures are intricately tied to the evolutionary processes of galaxies, including their star formation (SF) history and Active Galactic Nuclei (AGN) activities. Nevertheless, the precise origins and connections between the formation of warps, bars, and the evolution of galaxies remain shrouded in uncertainty. To address this critical endeavor, we have employed newly developed automated schemes for the identification of these morphological features. Our objective is to elucidate the interplay between star formation and AGN activities, and the genesis and evolution of warps and bars, drawing from empirical observations.
In the first part of this thesis, we investigate the origin of different two morpholo- gies: S- and U-type warps. Conventional theories routinely attribute both types to galactic tidal interaction and/or gas accretion, but reproducing of U-types in simu- lations is extremely challenging. Here we investigate whether both types are gov- erned by the same mechanisms using the most extensive sample of ∼8000 nearby (0.02 < z < 0.06) massive (M∗/M⊙ > 109) edge-on disks from SDSS. We find that U-types show on average bluer optical colors and higher specific star formation rate (sSFR) than S-types, with more strongly warped U-types having higher sSFR. We also find that while the S-type warp properties correlate with the tidal force by the nearest neighbor regardless of the environment, there is no such correlation for U- types in groups/clusters, suggesting a non-tidal environmental could be at play for U-types, such as ram pressure stripping (RPS). Indeed, U-types are more common in groups/clusters than in fields and they have stellar mass, gas fraction, sSFR enhancement and kinematics closely analogous to RPS-induced jellyfish galaxies. We furthermore show that the stellar disks of most RPS galaxies in the IllustirsTNG simulation are warped in U-shape and bent in opposite direction of stripped gas tails, satisfying theoretical expectations for stellar warps embeded in jellyfishes. We therefore suggest that despite U-types in fields being still less explained, RPS can be an alternative origin for those in groups/clusters.
In the second part, we unravel the interplay between bars, SF, and AGNs in barred galaxies. To this end, we utilize the SDSS DR12 to select a sample of nearby (0.02<!-- Not Allowed Tag Filtered --><z><0.06)diskgalaxiesthataresuitableforbarexamination(Mr <−20.12 and inclination ≲ 53◦). We identify 3662 barred galaxies and measure the length and axis ratio of each bar. We invent new bar parameters that mitigate the stellar and bulge mass biases and show, for the first time, that the evolution of non-AGN and AGN-hosting barred galaxies should be tracked using different bar parameters; the bar length for non-AGN galaxies and the bar axis ratio for AGN-hosting galax- ies. Our analysis confirms that barred galaxies have a higher specific SF rate than unbarred control galaxies. Moreover, we find a positive correlation of bar length with both the SF enhancement and the centrally star-forming galaxy fraction, indi- cating the interconnectivity of bars and SF through the bar-driven gas inflow. We also find that while the AGN fraction of barred galaxies is the same as that of the unbarred control sample, galaxies hosting more massive black holes (BHs) have rounder (i.e., higher axis ratio) bars, implying that the bar is not a cause of AGN activity; rather, AGNs appear to regulate bars. Our findings corroborate theoretical predictions that bars in non-AGN galaxies grow in length, and bars in AGN-hosting galaxies become rounder as BHs grow and eventually get destroyed.
In the third part, we delve into the impact of relative spin orientation on interaction- induced star formation (SF) in galaxy pairs through hydrodynamical processes. Utilizing data from the SDSS DR7 combined with the Galaxy Zoo 2 classification, we meticulously assemble a comprehensive sample of nearby spiral+spiral galaxies (0.02 < z < 0.06) along with an isolated control sample. Our prior re- search highlighted the role of hydrodynamical processes in enhancing SF in galaxy pairs, particularly evident when these galaxies are situated near star-forming neigh- bors. Re-examining this finding, we corroborate these results specifically within the context of spiral+spiral pairs. Furthermore, leveraging an innovative method to as- sess spin-spin alignment observationally, we systematically analyze the extent of interaction-induced SF in relation to spin-spin alignments. Notably, our results in- dicate that interaction-induced SF intensifies as the configuration of a pair system transitions from perpendicular to closely aligned. To account for this pronounced SF in well-aligned systems, we propose two potential mechanisms: the heightened hydrodynamical friction attributed to ram-pressure in such aligned configurations, and the inclination towards prograde orbits, which typically stimulate more SF in well-aligned pairs
In summary, morphological features of disk galaxies serve as valuable indicators of galactic evolution. Our research has unveiled distinct formation mechanisms for S- and U-type warps. S-shaped warped galaxies predominantly arise from galaxy- galaxy tidal interactions, whereas some U-shaped warped galaxies can be attributed to ram-pressure stripping, particularly within galaxy cluster/group environments. In the case of galactic bars, our investigations have revealed a systematic evolutionary trajectory from non-AGN barred galaxies to AGN barred galaxies. Bars within non- AGN barred galaxies undergo growth driven by gas inflow, which, in turn, triggers enhanced star formation. Conversely, bars in AGN barred galaxies experience a process of weaken due to the expansion of central BHs. The interaction-induced SFR depends on the relative orientation of spins of galaxy pairs. Well-aligned pair systems exhibit stronger enhanced SF activity than less-aligned pairs, and this result can be explained by the result driven by the hydrodynamical process. Building upon our results, we offer insights into the link between the evolution of galaxies and these three prominent morphological features observed in disk galaxies: (a) warps, which manifest in edge-on galaxies, (b ) bars, which are evident in face-on galaxies, and (c) relative spin orientations of two paired galaxies.

목차 (Table of Contents)

• 1 Introduction
• 1.1 An Overview of Morphologies
• 1.1.1 Quantifying the Morphology of Galaxies
• 1.1.2 The Bimodality of Morphologies
• 1.2 Outer structures of Edge-on Disks: Warps
• 1.2.1 Milky Way’s Warp
• 1.2.2 Warps in Disk Galaxies
• 1.2.3 The Structure of Galactic Warps
• 1.2.4 Disputing the Origin of Galactic Warps
• 1.3 Inner Structures of Face-on Disks: Bars
• 1.3.1 Milky Way’s Bar
• 1.3.2 Bars in Disk Galaxies
• 1.3.3 The Evolution of Galactic Bars
• 1.3.4 Links between Active Galactic Nuclei and Bars
• 1.4 Spin Orientation of Disk Galaxies
• 1.4.1 Intrinsic Spin and Tidal Torque Fields
• 1.4.2 Spin Orientation and the Evolution of Galaxy Pairs
• 1.5 Thesis Objectives and Outline
• 2 A Possible Link between Jellyfish Galaxies and the Origin of U-type Warps
• 2.1 Introduction
• 2.2 Data and Methodology
• 2.2.1 Observational Data
• 2.2.2 Measurements of the Warped Stellar Disks
• 2.2.3 Warped Disk Galaxy Sample
• 2.2.4 Control Sample
• 2.3 Physical Properties of Warped Disk Galaxies
• 2.3.1 The Optical Color and Star Formation Rate
• 2.3.2 TheEnvironment
• 2.4 Are U-type warps in groups/clusters jellyfishes?
• 2.4.1 Warped Jellyfish Galaxies
• 2.4.2 The Phase-Space Distribution of Group/Cluster Galaxies
• 2.4.3 Stellar Mass, Star Formation Rate, and Gas Mass Fraction
• 2.5 SummaryandDiscussion
• 3 Bar Growth in Star-forming and Bar Dissolution in AGN-hosting Galaxies
• 3.1 Introduction
• 3.2 Dataand Methodology
• 3.2.1 Observational Data
• 3.2.2 Bar Classification and Measurements
• 3.2.3 Control Sample
• 3.3 New Bar Parameters
• 3.3.1 The Dependence of Bar Properties
• 3.3.2 The Definition ofNewBar Parameters
• 3.4 Interplay of Bars with SF and AGNs
• 3.4.1 Interplay between Bars and SF Activities for Non-AGN Galaxies
• 3.4.2 Interplay between Bars and BH Activities for AGN Galaxies
• 3.4.3 The Difference between Isolated and Tidally Triggered Bars
• 3.5 Summary and Conclusions
• 4 Augmented Star Formation in Well-Aligned Spiral+Spiral Pairs
• 4.1 Introduction
• 4.2 Dataand Methodology
• 4.2.1 Observational Data
• 4.2.2 Identification of Spiral+Spiral Pairs
• 4.2.3 Relative SF Activities of the Nearest Neighbors
• 4.2.4 MeasurementofSpin-SpinAlignment
• 4.2.5 ControlSample
• 4.3 Results
• 4.3.1 Revisiting Tidal & Hydrodynamical Effects: Closer and Bluer Neighbors Enhance SF
• 4.3.2 Augmentation of Interaction-Induced SF in Well-Aligned PairSystems
• 4.4 Discussion
• 4.4.1 Does Well-Aligned Configuration Result from Interactions that Enhance SF?
• 4.4.2 How Does Alignment Enhance SF During Interaction?
• 4.5 Summary and Conclusions
• 5 Conclusion
• 5.1 SummaryandConclusion
• 5.2 FutureDirections
• 5.2.1 A Link between Dark Matter Halos and Galactic Warps
• 5.2.2 The Next Chapter of Galactic Anatomy: Spiral Arms

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