Advances in constraining intrinsic alignment models with hydrodynamic simulations

ABSTRACT We use galaxies from the illustristng, massiveblack-ii, and illustris-1 hydrodynamic simulations to investigate the behaviour of large scale galaxy intrinsic alignments. Our analysis spans four redshift slices over the approximate range of contemporary lensing surveys z = 0−1. We construct comparable weighted samples from the three simulations, which we then analyse using an alignment model that includes both linear and quadratic alignment contributions. Our data vector includes galaxy–galaxy, galaxy–shape, and shape–shape projected correlations, with the joint covariance matrix estimated analytically. In all of the simulations, we report non-zero IAs at the level of several σ. For a fixed lower mass threshold, we find a relatively strong redshift dependence in all three simulations, with the linear IA amplitude increasing by a factor of ∼2 between redshifts z = 0 and z = 1. We report no significant evidence for non-zero values of the tidal torquing amplitude, A2, in TNG, above statistical uncertainties, although MBII favours a moderately negative A2 ∼ −2. Examining the properties of the TATT model as a function of colour, luminosity and galaxy type (satellite or central), our findings are consistent with the most recent measurements on real data. We also outline a novel method for constraining the TATT model parameters directly from the pixelized tidal field, alongside a proof-of-concept exercise using TNG. This technique is shown to be promising, although comparison with previous results obtained via other methods is non-trivial.

Search for gas accretion imprints in voids: II. The galaxy Ark 18 as a result of a dwarf-dwarf merger

The low-mass low-surface brightness (LSB) disc galaxy Arakelian 18 (Ark 18) resides in the Eridanus void and because of its isolation represents an ideal case to study the formation and evolution mechanisms of such a galaxy type. Its complex structure consists of an extended blue LSB disc and a bright central elliptically-shaped part hosting a massive off-centered star-forming clump. We present the in-depth study of Ark 18 based on observations with the SCORPIO-2 long-slit spectrograph and a scanning Fabry-Perot interferometer at the Russian 6-m telescope complemented by archival multi-wavelength images and SDSS spectra. Ark 18 appears to be a dark matter dominated gas-rich galaxy without a radial metallicity gradient. The observed velocity field of the ionised gas is well described by two circularly rotating components moderately inclined with respect to each other and a possible warp in the outer disc. We estimated the age of young stellar population in the galaxy centre to be ∼140 Myr, while the brightest star-forming clump appears to be much younger. We conclude that the LSB disc is likely the result of a dwarf–dwarf merger with a stellar mass ratio of the components at least ∼5:1 that occurred earlier than 300 Myr ago. The brightest star forming clump was likely formed later by accretion of a gas cloud.

I- A hydrodynamical Clone of the Virgo cluster of galaxies to confirm observationally-driven formation scenarios

At ∼16-17 Mpc from us, the Virgo cluster is a formidable source of information to study cluster formation and galaxy evolution in rich environments. Several observationally-driven formation scenarios arose within the past decade to explain the properties of galaxies that entered the cluster recently and the nature of the last significant merger that the cluster underwent. Confirming these scenarios requires extremely faithful numerical counterparts of the cluster. This paper presents the first Clone, Constrained LOcal and Nesting Environment, simulation of the Virgo cluster within a ∼15 Mpc radius sphere. This cosmological hydrodynamical simulation, with feedback from supernovae and active galactic nuclei, with a ∼3 × 107 M⊙ dark matter particle mass and a minimum cell size of 350 pc in the zoom region, reproduces Virgo within its large scale environment unlike a random cluster simulation. Overall the distribution of the simulated galaxy population matches the observed one including M87. The simulated cluster formation reveals exquisite agreements with observationally-driven scenarios: within the last Gigayear, about 300 small galaxies (M*>107 M⊙) entered the cluster, most of them within the last 500 Myr. The last significant merger event occurred about 2 Gigayears ago: a group with a tenth of the mass of today’s cluster entered from the far side as viewed from the Milky Way. This excellent numerical replica of Virgo will permit studying different galaxy type evolution (jellyfish, backsplash, etc.) as well as feedback phenomena in the cluster core via unbiased comparisons between simulated and observed galaxies and hot gas phase profiles to understand this great physics laboratory.

Classifying stars, galaxies, and AGNs in CLAUDS + HSC-SSP using gradient boosted decision trees

ABSTRACT Classifying catalogue objects as stars, galaxies, or active galactic nuclei (AGNs) is a crucial part of any statistical study of galaxies. We describe our pipeline for binary (star/galaxy) and multiclass (star/galaxy/Type I AGN/Type II AGN) classification developed for the very deep CLAUDS + HSC-SSP u*grizy data set. Our method uses the XGBoost implementation of gradient boosted trees (GBTs) to train ensembles of models that take photometry, colours, maximum surface brightnesses, and effective radii from all available bands as input, and output the probability that an object belongs to each of the classes under consideration. At iAB < 25 our binary star/galaxy model has AUC = 0.9974 and at the threshold that maximizes our sample’s weighted F1 score, selects a sample of galaxies with 99.7 per cent purity and 99.8 per cent completeness. We test the model’s ability to generalize to objects fainter than those seen during training and find that extrapolation of ∼1−2 mag is reasonable for most applications provided that the galaxies in the training sample are representative of the range of redshifts and colours of the galaxies in the target sample. We also perform an exploratory analysis of the method’s ability to identify AGNs using a small X-ray-selected sample and find that it holds promise for classifying Type I AGN, although it performs less well for Type II AGN. Our results demonstrate that GBTs provide a flexible, robust, and efficient method for performing classification of catalogue objects in large astronomical imaging surveys.

A Novel Approach for Effective Alteration of Morphological Features of Polyaniline through Interfacial Polymerization for Versatile Applications

Morphological characteristics of any nanomaterial are critical in defining its properties. In this context, a method to control morphological parameters of polyaniline (PANI) has been investigated by producing its composite with gold nanoparticles (AuNPs). Herein, we report for the first time the successful control on the physical/chemical properties of PANI composites synthesized via interfacial polymerization through functionalization of its AuNP composite component with citrate, ascorbate, glutathione (GSH), and cetyl trimethyl ammonium bromide (CTAB). A significant difference in the polymerization pattern, morphologies, and electrical properties was recognized in these composites according to the functionality of the modified AuNPs. The obtained composites of AuNPs/PANI exhibited highly diverse morphologies (e.g., nodule, hollow hemisphere, flake, and spider-web galaxy type) and electrical characteristics according to functionalization. Hence, this study is expected to offer better insight into control of the polymerization pattern of AuNP/PANI composites and their associated properties.

The SAMI–Fornax Dwarfs Survey I: sample, observations, and the specific stellar angular momentum of dwarf elliptical galaxies

ABSTRACT Dwarf ellipticals are the most common galaxy type in cluster environments; however, the challenges associated with their observation mean that their formation mechanisms are still poorly understood. To address this, we present deep integral field observations of a sample of 31 low-mass (107.5 < M⋆ < 109.5 M⊙) early-type galaxies in the Fornax cluster with the SAMI instrument. For 21 galaxies, our observations are sufficiently deep to construct spatially resolved maps of the stellar velocity and velocity dispersion – for the remaining galaxies, we extract global velocities and dispersions from aperture spectra only. From the kinematic maps, we measure the specific stellar angular momentum λR of the lowest mass dE galaxies to date. Combining our observations with early-type galaxy data from the literature spanning a large range in stellar mass, we find that λR decreases towards lower stellar mass, with a corresponding increase in the proportion of slowly rotating galaxies in this regime. The decrease of λR with mass in our sample dE galaxies is consistent with a similar trend seen in somewhat more massive spiral galaxies from the CALIFA survey. This suggests that the degree of dynamical heating required to produce dEs from low-mass starforming progenitors may be relatively modest and consistent with a broad range of formation mechanisms.

Dust properties and star formation of approximately a thousand local galaxies

Aims. We derived the dust properties for 753 local galaxies and examine how these relate to some of their physical properties. We present the derived dust emission properties, including model spectral energy distribution (SEDs), star formation rates (SFRs) and stellar masses, as well as their relations. Methods. We modelled the global dust-SEDs for 753 galaxies, treated statistically as an ensemble within a hierarchical Bayesian dust-SED modelling approach, so as to derive their infrared (IR) emission properties. To create the observed dust-SEDs, we used a multi-wavelength set of observations, ranging from near-IR to far-IR-to-submillimeter wavelengths. The model-derived properties are the dust masses (Mdust), the average interstellar radiation field intensities (Uav), the mass fraction of very small dust grains (“QPAH” fraction), as well as their standard deviations. In addition, we used mid-IR observations to derive SFR and stellar masses, quantities independent of the dust-SED modelling. Results. We derive distribution functions of the properties for the galaxy ensemble and as a function of galaxy type. The mean value of Mdust for the early-type galaxies (ETGs) is lower than that for the late-type and irregular galaxies (LTGs and Irs, respectively), despite ETGs and LTGs having stellar masses spanning across the whole range observed. The Uav and “QPAH” fraction show no difference among different galaxy types. When fixing Uav to the Galactic value, the derived “QPAH” fraction varies across the Galactic value (0.071). The specific SFR increases with galaxy type, while this is not the case for the dust-specific SFR (SFR/Mdust), showing an almost constant star formation efficiency per galaxy type. The galaxy sample is characterised by a tight relationship between the dust mass and the stellar mass for the LTGs and Irs, while ETGs scatter around this relation and tend towards smaller dust masses. While the relation indicates that Mdust may fundamentally be linked to M⋆, metallicity and Uav are the second parameter driving the scatter, which we investigate in a forthcoming work. We used the extended Kennicutt–Schmidt (KS) law to estimate the gas mass and the gas-to-dust mass ratio (GDR). The gas mass derived from the extended KS law is on average ∼20% higher than that derived from the KS law, and a large standard deviation indicates the importance of the average star formation present to regulate star formation and gas supply. The average GDR for the LTGs and Irs is 370, and including the ETGs gives an average of 550.

Pemanfaatan Mobile Base Station South Tipe Galaxy G1 untuk Pengukuran Titik Batas Bidang Tanah

Implementation of land measurement using CORS / JRSP has constraints, namely the limited availability of base stations, resulting in unreachable areas. Rapid technological developments enable base stations are brought directly in the mesaurement location. The technology is called mobile base station. The purpose of this study is to 1) test whether there is a significant difference between the coordinates of the land Parcels boundary point using Mobile Base station South Type Galaxy G1 to CORS / JRSP and Static (Post Processing) coordinate values, 2) test the accuracy of the measurement results using Mobile Base station South Type Galaxy G1 against CORS / JRSP and Static (Post Processing).The research method that has been used is experiment with comparative experiment with quantitative approach. The sample is divided into 2 categories that is in therange of 5-10 Km and 10-15 Km from base station of Land Office of Sleman Regency. Data were analyzed using t test at significance level (?) 5%.Based on the analysis performed, it is known 1) At 5% significance level there are no significant difference between the coordinate values that are resulted by using Mobile Base Station South type Galaxy G1 using CORS / JRSP and using Static (Post Processing) in range 5-10 Km and 10-15 Km from Base station. but the coordinate value that are resulted by using Mobile Base Station South type Galaxy G1 using CORS / JRSP are not fulfilling the tolerance according to PMNA / KBPN Number 3 Year 1997. 2) The accuracy of coordinates value using Mobile Base station South Galaxy type G1 are smaller than with CORS / JRSP but greater than Static (Post Processing) based on horizontal accuracy parameter (HRMS). Keywords: CORS/JRSP, Mobile Base station, SOUTH Galaxy G1 Intisari: Pada pelaksanaan pengukuran bidang tanah menggunakan CORS/JRSP terdapat hambatan yaitu terbatasnya ketersediaan base station, mengakibatkan adanya wilayah yang tidak terjangkau. Kemajuan teknologi yang pesat memungkinkan base station dapat dibawa langsung di lapangan. Teknologi tersebut dinamakan mobile base station. Tujuan dari penelitian ini adalah untuk 1) menguji apakah terdapat perbedaan yang signifikan antara koordinat hasil pengukuran titik batas bidang tanah menggunakan Mobile Base station South Tipe Galaxy G1 terhadap nilai koordinat CORS/JRSP dan Statik (Post Processing), 2) menguji ketelitian hasil pengukuran menggunakan Mobile Base station South Tipe Galaxy G1 terhadap CORS/JRSP dan Statik (Post Processing). Metode penelitian yang digunakan adalah percobaan dengan perbandingan (comparative experiment) dengan pendekatan kuantitatif. Sampel terbagi dalam 2 kategori yaitu pada jangkauan 5-10 Km dan 10-15 Km dari base station Kantor Pertanahan Kabupaten Sleman. Analisis data dilakukan dengan Uji t pada taraf signifikansi (?) 5%. Berdasarkan analisis yang dilakukan, maka diketahui 1) Perbedaan nilai koordinat Mobile Base station South tipe Galaxy G1 terhadap nilai koordinat CORS/JRSP dan Statik (Post Processing) pada jangkauan 5-10 Km dan 10-15 Km dari Base station Kantor Pertanahan Kabupaten Sleman berdasarkan hasil uji t dengan taraf signifikansi 5% tidak berbeda signifikan akan tetapi tidak memenuhi toleransi sesuai dengan PMNA/KBPN Nomor 3 Tahun 1997, 2) Ketelitian hasil pengukuran berdasarkan parameter ketelitian horizontal (HRMS) didapatkan hasil yaitu ketelitian Mobile Base station South tipe Galaxy G1 lebih kecil dibandingkan dengan CORS/JRSP akan tetapi lebih besar dibandingkan dengan Statik (Post Processing). Kata Kunci: CORS/JRSP, Mobile Base station, SOUTH Galaxy G1

The Leo-I group: new dwarf galaxy and ultra diffuse galaxy candidates

Context. The study of dwarf galaxies and their environments provides crucial test beds for predictions of cosmological models and insights into the structure formation on small cosmological scales. In recent years, many problems on the scale of groups of galaxies has challenged the current standard model of cosmology. Aims. Our aim is to increase the sample of known galaxies in the Leo-I group, which contains the M 96 subgroup and the Leo Triplet. This galaxy aggregate is located at the edge of the Local Volume at a mean distance of 10.7 Mpc. Methods. We employed image enhancing techniques to search for low surface brightness objects in publicly available gr images taken by the Sloan Digital Sky Survey within 500 square degrees around the Leo-I group. Once detected, we performed surface photometry and compared their structural parameters to other known dwarf galaxies in the nearby universe. Results. We found 36 new dwarf galaxy candidates within the search area. Their morphology and structural parameters resemble known dwarfs in other groups. Among the candidates five or six galaxies are considered as ultra diffuse galaxy candidates. If confirmed, they would be some of the closest examples of this galaxy type. We assessed the luminosity function of the Leo-I group and find it to be considerably rich in dwarf galaxies, with twice the number of galaxies as the Local Group at a limiting magnitude of MV = −10 and a steeper faint-end slope.