GAMA/H-ATLAS: A meta-analysis of SFR indicators - comprehensive measures of the SFR-M* relation and Cosmic Star Formation History at z < 0.4
L. J. M. Davies, S. P. Driver, A. S. G. Robotham, M. W. Grootes, C. C. Popescu, R. J. Tuffs, A. Hopkins, M. Alpaslan, S. K. Andrews, J. Bland-Hawthorn, M. N. Br… 展开作者
L. J. M. Davies, S. P. Driver, A. S. G. Robotham, M. W. Grootes, C. C. Popescu, R. J. Tuffs, A. Hopkins, M. Alpaslan, S. K. Andrews, J. Bland-Hawthorn, M. N. Bremer, S. Brough, M. J. I. Brown, M. E. Cluver, S. Croom, E. da Cunha, L. Dunne, M. A. Lara-Lopez, J. Liske, J. Loveday, A. J. Moffett, M. Owers, S. Phillipps, A. E. Sansom, E. N. Taylor, M. J. Michalowski, E. Ibar, M. Smith, N. Bourne
我们对GAMA调查中的恒星形成率（SFR）指标进行了荟萃分析，产生了12个不同的SFR指标，并确定了每个指标的SFR-M * 关系。我们比较和对比已发表的方法，以提取SFR从每个指标，使用一个定义明确的本地样本的形态选择的螺旋星系，其中不包括来源，可能有大的最近的变化，他们的SFR。不同的方法被发现产生SFR-M* 关系与不一致的斜率和归一化，表明校准方法之间的差异。恢复的SFR-M* 关系也具有大范围的散射，这是因为目标的SFR可以被认为在不同的时间尺度上是恒定的，这表明方法校正单个目标中的衰减的准确度的差异。然后，我们重新校准所有的SFR指标，以提供新的，强大的和一致的亮度SFR校准，发现最一致的斜率和归一化的SFR-M * 的关系时，重新校准使用辐射传输方法Popescu等。这些新的校准可以用来直接比较SFR在不同的观测，历元和星系种群。然后，我们将我们的校准GAMA II赤道数据集，并探讨在本地宇宙的恒星形成的演变。我们确定从0 < z < 0.35到SFR-M* 关系的归一化的演变-在0.3 < z < 1.2时发现与先前估计一致的趋势。然后，我们提供了z < 0.35的宇宙恒星形成历史，SFR-M* 关系及其在过去30亿年的演化。
英文摘要：
We present a meta-analysis of star-formation rate (SFR) indicators in the GAMA survey, producing 12 different SFR metrics and determining the SFR-M* relation for each. We compare and contrast published methods to extract the SFR from each indicator, using a well-defined local sample of morphologically-selected spiral galaxies, which excludes sources which potentially have large recent changes to their SFR. The different methods are found to yield SFR-M* relations with inconsistent slopes and normalisations, suggesting differences between calibration methods. The recovered SFR-M* relations also have a large range in scatter which, as SFRs of the targets may be considered constant over the different timescales, suggests differences in the accuracy by which methods correct for attenuation in individual targets. We then recalibrate all SFR indicators to provide new, robust and consistent luminosity-to-SFR calibrations, finding that the most consistent slopes and normalisations of the SFR-M* relations are obtained when recalibrated using the radiation transfer method of Popescu et al. These new calibrations can be used to directly compare SFRs across different observations, epochs and galaxy populations. We then apply our calibrations to the GAMA II equatorial dataset and explore the evolution of star-formation in the local Universe. We determine the evolution of the normalisation to the SFR-M* relation from 0 < z < 0.35 - finding consistent trends with previous estimates at 0.3 < z < 1.2. We then provide the definitive z < 0.35 Cosmic Star Formation History, SFR-M* relation and its evolution over the last 3 billion years.
We study the star formation rate (SFR), stellar mass ($M_{\star}$) and the gas metallicity (Z) for 4,636 galaxy pairs using the Galaxy And Mass Assembly (GAMA) survey. Our galaxy pairs lie in a redshift range of 0 $<$ $z$ $<$ 0.35, mass range of 7.5 $<$ log( M$_{\star}$/ M$_\odot$) $<$ 11.5 and $ΔV$ $<$ 1000 km s$^{-1}$. We explore variations in SFR and Z from three point of views: multiplicity, pair separation and dynamics. We define multiplicity as the number of galaxies paired with a single galaxy, and analyzed for the first time variations in SFR and Z for both, single pairs and pairs with…
We present a study of the relationships and environmental dependencies between stellar mass, star formation rate, and gas metallicity for more than 700 galaxies in groups up to redshift 0.35 from the Galaxy And Mass Assembly (GAMA) survey. To identify the main drivers, our sample was analyzed as a function of group-centric distance, projected galaxy number density, and stellar mass. By using control samples of more than 16000 star-forming field galaxies and volume limited samples, we find that the highest enhancement in SFR (0.3 dex) occurs in galaxies with the lowest local density. In contras…
Recently a number of studies have proposed that the dispersion along the star formation rate - stellar mass relation ($σ_{\mathrm{sSFR}}$-M$_{*}$) is indicative of variations in star-formation history (SFH) driven by feedback processes. They found a 'U'-shaped dispersion and attribute the increased scatter at low and high stellar masses to stellar and active galactic nuclei feed-back respectively. However, measuring $σ_{\mathrm{sSFR}}$ and the shape of the $σ_{\mathrm{sSFR}}$-M$_{*}$ relation is problematic and can vary dramatically depending on the sample selected, chosen separation of passiv…
We describe data release 3 (DR3) of the Galaxy And Mass Assembly (GAMA) survey. The GAMA survey is a spectroscopic redshift and multi-wavelength photometric survey in three equatorial regions each of 60.0 deg^2 (G09, G12, G15), and two southern regions of 55.7 deg^2 (G02) and 50.6 deg^2 (G23). DR3 consists of: the first release of data covering the G02 region and of data on H-ATLAS sources in the equatorial regions; and updates to data on sources released in DR2. DR3 includes 154809 sources with secure redshifts across four regions. A subset of the G02 region is 95.5% redshift complete to r<19…
We explore how the group environment may affect the evolution of star-forming galaxies. We select 1197 Galaxy And Mass Assembly (GAMA) groups at $0.05\leq z \leq 0.2$ and analyze the projected phase space (PPS) diagram, i.e. the galaxy velocity as a function of projected group-centric radius, as a local environmental metric in the low-mass halo regime $10^{12}\leq (M_{200}/M_{\odot})< 10^{14}$. We study the properties of star-forming group galaxies, exploring the correlation of star formation rate (SFR) with radial distance and stellar mass. We find that the fraction of star-forming group memb…
EMU/GAMA: Refining Dust Extinction Corrections for Hα Luminosity Functions Using Radio-Based Calibration
Macquarie University（麦考瑞大学）；Universidade de Lisboa（里斯本大学）；Australian Astronomical Optics（澳大利亚天文光学）；Western Sydney University（西悉尼大学）；Australian National University（澳大利亚国立大学）；Ruhr Astroparticle and Plasma Physics Center (RAPP Center)（鲁尔亚原子与等离子体物理中心（RAPP中心））；Monash University（莫纳什大学）；Queensland University of Technology（昆士兰科技大学）；University of Hawai’i at Mānoa（夏威夷大学马诺阿分校）；Curtin University（科廷大学）
We present measurements of the angular correlation function of sub-millimeter (sub-mm) galaxies (SMGs) identified in four out of the five fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) - GAMA-9h, GAMA-12h, GAMA-15h and NGP - with flux densities $S_{250μm}$>30 mJy at 250 μm. We show that galaxies selected at this wavelength trace the underlying matter distribution differently at low and high redshifts. We study the evolution of the clustering finding that at low redshifts sub-mm galaxies exhibit clustering strengths of $r_0$ $\sim$ 2 - 3 $h^{-1}$ Mpc, below z < 0.3. …
We present the dust mass function (DMF) of 15,750 galaxies with redshift $z< 0.1$, drawn from the overlapping area of the GAMA and {\it H-}ATLAS surveys. The DMF is derived using the density corrected $V_{\rm max}$ method, where we estimate $V_{\rm max}$ using: (i) the normal photometric selection limit ($pV_{\rm max}$) and (ii) a bivariate brightness distribution (BBD) technique, which accounts for two selection effects. We fit the data with a Schechter function, and find $M^{*}=(4.65\pm0.18)\times 10^{7}\,h^2_{70}\, M_{\odot}$, $α=(1.22\pm 0.01)$, $ϕ^{*}=(6.26\pm 0.28)\times 10^{-3}\,h^3_{70…
Aims. We aim to investigate if the environment (characterised by the host dark matter halo mass) plays any role in shaping the galaxy star formation main sequence (MS). Methods. The Galaxy and Mass Assembly project (GAMA) combines a spectroscopic survey with photometric information in 21 bands from the far-ultraviolet (FUV) to the far-infrared (FIR). Stellar masses and dust-corrected star-formation rates (SFR) are derived from spectral energy distribution (SED) modelling using MAGPHYS. We use the GAMA galaxy group catalogue to examine the variation of the fraction of star-forming galaxies (SFG…
H-ATLAS/GAMA: Quantifying the Morphological Evolution of the Galaxy Population Using Cosmic Calorimetry
利用Herschel天体物理太赫兹大面积巡天和星系与质量组装项目的结果，我们表明，对于质量大于约1.0e8太阳质量的星系，本机宇宙中51%的恒星质量密度位于早型星系中（ETG：Sersic n > 2.5），而89%的恒星质量密度产生率发生在晚型星系（LTG：Sersic n < 2.5）。从这个零红移的基准，我们已经使用了量热技术来量化的重要性的形态转变的星系在宇宙的历史。河外背景辐射包含了大爆炸以来恒星核聚变产生的全部能量。通过使用赫歇尔空间天文台的最深远红外调查和哈勃太空望远镜（HST）的深近红外/光学调查将这种背景辐射分解为单个星系，并使用来自HST图像的这些星系的Sersic指数的测量值，我们估计在宇宙历史上形成的恒星质量密度中约有83%发生在LTG中。这与现今LTG中恒星质量密度的比例之间的差异意味着在大多数恒星形成之后，LTG必须有一个主要的转变。
We analyse the metallicity histories of ~4,500 galaxies from the GAMA survey at z<0.06 modelled by the SED-fitting code ProSpect using an evolving metallicity implementation. These metallicity histories, in combination with the associated star formation histories, allow us to analyse the inferred gas-phase mass--metallicity relation. Furthermore, we extract the mass--metallicity relation at a sequence of epochs in cosmic history, to track the evolving mass--metallicity relation with time. Through comparison with observations of gas-phase metallicity over a large range of redshifts, we show tha…
Radio emission is a key indicator of star-formation activity in galaxies, but the radio luminosity-star formation relation has to date been studied almost exclusively at frequencies of 1.4 GHz or above. At lower radio frequencies the effects of thermal radio emission are greatly reduced, and so we would expect the radio emission observed to be completely dominated by synchrotron radiation from supernova-generated cosmic rays. As part of the LOFAR Surveys Key Science project, the Herschel-ATLAS NGP field has been surveyed with LOFAR at an effective frequency of 150 MHz. We select a sample from …
Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) III: [C II] as Tracer, Crisis of SFR, [O III]/[C II] at High-z, New Answers and New Questions
We present an atlas of ultraviolet and infrared images of ~15,750 local (d < 50 Mpc) galaxies, as observed by NASA's WISE and GALEX missions. These maps have matched resolution (FWHM 7.5'' and 15''), matched astrometry, and a common procedure for background removal. We demonstrate that they agree well with resolved intensity measurements and integrated photometry from previous surveys. This atlas represents the first part of a program (the z=0 Multi-wavelength Galaxy Synthesis) to create a large, uniform database of resolved measurements of gas and dust in nearby galaxies. The images and assoc…
We present catalogues of stellar masses, star formation rates, and ancillary stellar population parameters for galaxies spanning $0<z<9$ from the Deep Extragalactic VIsible Legacy Survey (DEVILS). DEVILS is a deep spectroscopic redshift survey with very high completeness, covering several premier deep fields including COSMOS (D10). Our stellar mass and star formation rate estimates are self-consistently derived using the spectral energy distribution (SED) modelling code ProSpect, using well-motivated parameterisations for dust attenuation, star formation histories, and metallicity evolution. W…
Herschel-ATLAS: Properties of dusty massive galaxies at low and high redshifts
我们提出了一个比较的物理性质的休息帧$250μ$ m选定的样本的大规模，尘埃星系从$0<z<5.3$。我们的样本包括文献中的29个高红移亚毫米星系（SMG）和赫歇尔-阿特拉斯的$z<0.5$上的843个尘埃星系，这些星系被选择为与SMG具有相似的恒星质量。$z>1$ SMG的平均SFR为$390^{+80}_{-70}\,$ M $_\odot$ yr $^{-1}$，是在恒星质量上与SMG匹配的低红移样本的SFR（$=3.3\pm{0.2}$ M $_\odot$ yr $^{-1}$）的120倍。与低红移尘埃星系的$(1.6\pm0.1)\times{10}^8\,$ M $_\odot$相比，SMG拥有大量的尘埃（$1.2^{+0.3}_{-0.2}\times{10}^9\,$ M $_\odot$）。在低红移的尘埃光度占主导地位的弥漫ISM，而大部分的尘埃光度的SMG起源于恒星形成区。在相同的尘埃质量的SMG是向更高的SFR相比，低红移的H-ATLAS星系偏移。这不仅是因为SMG中的气体比例较高，而且还因为它们正在经历一种更有效的恒星形成模式，这与它们的爆发性恒星形成历史相一致。SMG和低红移星系之间的SFR偏移与CO研究中发现的相似，这表明尘埃质量和CO一样是分子气体的良好示踪剂。
We study the physical properties of the ionized gas in local disks using the sample of 38 nearby $\sim10^{8.5-11.2}$M$_\odot$ Star-Forming Main Sequence (SFMS) galaxies observed so far as part of the MUSE Atlas of Disks (MAD). Specifically, we use all strong emission lines in the MUSE wavelength range 4650-9300 Å to investigate the resolved ionized gas properties on $\sim$100 pc scales. This spatial resolution enables us to disentangle HII regions from the Diffuse Ionized Gas (DIG) in the computation of gas metallicities and Star Formation Rates (SFRs) of star forming regions. The gas metallic…
We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved observations of molecular gas in galaxies up to $z=0.35$ to characterise the role of global galactic dynamics on the global interstellar medium (ISM) properties. These observations consist of a sub-sample of 39 galaxies taken from the Valparaíso ALMA Line Emission Survey (VALES). From the CO($J=1-0)$ emission line, we quantify the kinematic parameters by modelling the velocity fields. We find that the IR luminosity increases with the rotational to dispersion velocity ratio ($V_{\rm rot}/σ_v$, corrected for inclination). We…
We present a detailed analysis of the specific star formation rate -- stellar mass ($\mathrm{sSFR}-M_*$) of $z\le 0.13$ disk central galaxies using a morphologically selected mass-complete sample ($M_* \ge 10^{9.5} M_{\odot}$). Considering samples of grouped and ungrouped galaxies, we find the $\mathrm{sSFR}-M_*$ relations of disk-dominated central galaxies to have no detectable dependence on host dark-matter halo (DMH) mass, even where weak-lensing measurements indicate a difference in halo mass of a factor $\gtrsim5$. We further detect a gradual evolution of the $\mathrm{sSFR}-M_*$ relation …
We perform lens modelling and source reconstruction of Submillimeter Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$μ$m in the Herschel Astrophysical Terahertz Large Area Survey H-ATLAS. A previous analysis of the same dataset used a single Sèrsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from the H-ATLAS sampl…
Star Formation in Simulated Galaxies: Understanding the Transition to Quiescence at $3\times10^{10}$ M$_\odot$
星系中的恒星形成依赖于冷的致密气体的可用性，而这反过来又依赖于星系内部和外部的因素。为了提供一个简单的模型，恒星的形成是如何调节星系中的各种物理过程，我们分析了红移数据$z=0$从流体动力学宇宙学模拟，包括处方恒星形成和恒星演化，活动星系核（AGN），以及它们相关的反馈过程。该模型可以确定恒星形成率（SFR）作为星系恒星质量，气体质量，黑洞质量和环境的函数。我们发现，在低质量星系中，气体质量是控制恒星形成的最重要的量，并且在致密环境中的恒星形成星系比在该领域中的对应星系具有更高的SFR。在高质量星系中，我们发现质量大于$\sim10^{7.5}$ M $_\odot$的黑洞可以被触发，以淬灭其宿主中的恒星形成;这种质量尺度在我们的模拟中是涌现的。此外，这个黑洞质量对应于星系核球质量$\sim2\times10^{10}$ M $_\odot$，与早期类型星系开始占主导地位的质量（$\sim3\times10^{10}$ M $_\odot$，如考夫曼等人先前的观测所示）一致。最后，我们证明，我们的模型可以很好地再现从观测的星系在GAMA和ALOKFA调查的SFR测量。
Nonparametric star formation histories (SFHs) have long promised to be the `gold standard' for galaxy spectral energy distribution (SED) modeling as they are flexible enough to describe the full diversity of SFH shapes, whereas parametric models rule out a significant fraction of these shapes {\it a priori}. However, this flexibility is not fully constrained even with high-quality observations, making it critical to choose a well-motivated prior. Here, we use the SED-fitting code \texttt{Prospector} to explore the effect of different nonparametric priors by fitting SFHs to mock UV-IR photometr…
We study the environment in which a galaxy lies (i.e. field or group) and its connection with the morphology of the galaxy. This is done by examining the distribution of parametric and non-parametric statistics across the star-formation rate (SFR) - stellar mass (M$_{\star}$) plane and studying how these distributions change with the environment in the local universe ($z<0.15$). We determine the concentration (C), Gini, M$_{20}$, asymmetry, Gini-M$_{20}$ bulge statistic (GMB), 50\% light radius ($r_{50}$), total Sérsic index, and bulge Sérsic index ($n_{Bulge}$) for galaxies from the Galaxy an…
(Abridged) In this paper, we use the Tuffs et al. attenuation - inclination models in ultraviolet (UV), optical, and near-infrared (NIR) bands to investigate the average global dust properties in galaxies as a function of stellar mass $M_{*}$, stellar mass surface density $μ_{*}$, star-formation rate $SFR$, specific star-formation rate $sSFR$, star-formation main-sequence offset $dMS$, and star-formation rate surface density $Σ_{SFR}$ at redshifts $z \sim 0$ and $z \sim 0.7$. We use star-forming galaxies from SDSS ($\sim$ 20000) and GAMA ($\sim$ 2000) to form our low-z sample at $0.04 < z < 0.…
Far-ultraviolet (FUV; ~1200-2000 angstroms) spectra are fundamental to our understanding of star-forming galaxies, providing a unique window on massive stellar populations, chemical evolution, feedback processes, and reionization. The launch of JWST will soon usher in a new era, pushing the UV spectroscopic frontier to higher redshifts than ever before, however, its success hinges on a comprehensive understanding of the massive star populations and gas conditions that power the observed UV spectral features. This requires a level of detail that is only possible with a combination of ample wave…
VALES: I. The molecular gas content in star-forming dusty H-ATLAS galaxies up to z=0.35
我们提出了一个河外调查使用的观测从阿塔卡马大型毫米/亚毫米阵列（ALMA）的银河系人口高达$z=0.35$：瓦尔帕莱索ALMA线发射调查（VALES）。利用ALMA波段3 CO（1- 0）观测资料，研究了$Herschel$天体物理太赫兹大区域巡天（$H$-ATLAS）中67个尘埃正常恒星形成星系的分子气体含量。我们已经在$>5σ$显着性和其他12个星系的光谱检测到在堆叠光谱低的意义。CO的光度在$(0.03-1.31)\times10^{10}$ K km s $^{-1}$ pc $^2$的范围内，相当于$\log({\rm M_{gas}/M_{\odot}}) =8.9-10.9$假设一个$α_{\rm CO}$ =4.6（K km s $^{-1}$ pc $^{2}$）$^{-1}$，这完美地补充了以前探索的本地和高z正常星系的参数空间。我们计算了21个星系的光学CO尺寸比的ALMA解决$\sim 3$。“$5$分辨率（6.5 kpc），发现分子气体平均比恒星成分致密0.6倍。我们得到了一个整体的Schmidt-Kennicutt关系，由$\log [Σ_{\rm SFR}/({\rm M_{\odot} yr^{-1}kpc^{-2}})]=(1.26 \pm 0.02) \times \log [Σ_{\rm M_{H2}}/({\rm M_{\odot}\,pc^…
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies in the Local Universe I. - The Effect of the Group Environment on Star Formation in Spiral Galaxies
There is growing evidence supporting the coeval growth of galaxies and their resident SMBH. Most studies also claim a correlation between the activity of the SMBH and the star-formation of the host galaxy. It is unclear, though, whether this correlation extends to all redz and LX. In this work, we use data from the X-ATLAS and XMM-XXL North fields and compile the largest X-ray sample up to date, to investigate how X-ray AGN affect the star-formation of their host galaxies in a wide redz and luminosity baseline, i.e., 0.03<z<3 and log LX (2-10 keV)= (41-45.5) ergs-1. Our sample consists of 3336…
Parametric models for galaxy star-formation histories (SFHs) are widely used, though they are known to impose strong priors on physical parameters. This has consequences for measurements of the galaxy stellar-mass function (GSMF), star-formation-rate density (SFRD) and star-forming main sequence (SFMS). We investigate the effects of the exponentially declining, delayed exponentially declining, lognormal and double power law SFH models using BAGPIPES. We demonstrate that each of these models imposes strong priors on specific star-formation rates (sSFRs), potentially biasing the SFMS, and also i…
The Square Kilometer Array (SKA) is expected to detect high-redshift galaxies with star formation rates (SFRs) up to two orders of magnitude lower than Herschel surveys and will thus boost the ability of radio astronomy to study extragalactic sources. The tight infrared-radio correlation offers the possibility of using radio emission as a dust-unobscured star formation diagnostic. However, the physics governing the link between radio emission and star formation is poorly understood, and recent studies have pointed to differences in the exact calibration required when radio is to be used as a s…
We characterize the ionized gas outflows in 15 low-redshift star-forming galaxies, a Valparaíso ALMA Line Emission Survey (VALES) subsample, using MUSE integral field spectroscopy and GAMA photometric broadband data. We measure the emission-line spectra by fitting a double-component profile, with the second and broader component being related to the outflowing gas. This interpretation is in agreement with the correlation between the observed star-formation rate surface density ($Σ_{\mathrm{SFR}}$) and the second-component velocity dispersion ($σ_{\mathrm{2nd}}$), expected when tracing the feed…
The Central Molecular Zone (CMZ), a $\sim$200 pc sized region around the Galactic Centre, is peculiar in that it shows a star formation rate (SFR) that is suppressed with respect to the available dense gas. To study the SFR in the CMZ, young stellar objects (YSOs) can be investigated. Here we present radio observations of 334 2.2 $μ$m infrared sources that have been identified as YSO candidates. Our goal is to investigate the presence of centimetre wavelength radio continuum counterparts to this sample of YSO candidates which we use to constrain the current SFR in the CMZ. As part of the GLOST…
We introduce a novel abundance matching technique that produces a more accurate estimate of the pre-infall halo mass, $M_{200}$, for satellite galaxies. To achieve this, we abundance match with the mean star formation rate, averaged over the time when a galaxy was forming stars, $\langle {\rm SFR}\rangle$, instead of the stellar mass, $M_*$. Using data from the Sloan Digital Sky Survey, the GAMA survey and the Bolshoi simulation, we obtain a statistical $\langle {\rm SFR}\rangle-{\rm M}_{200}$ relation in $Λ{\rm CDM}$. We then compare the pre-infall halo mass, $M^{\rm abund}_{200}$, derived fr…
We examine the far-IR properties of a sample of 5391 optically selected QSOs in the 0.5<z<2.65 redshift range down to log[nuLnu,2500 (erg/s)]>44.7, using SPIRE data from Herschel-ATLAS. We split the sample in a grid of 74 luminosity-redshift bins and compute the average optical-infrared spectral energy distribution (SED) in each bin. By normalising an intrinsic AGN template to the AGN optical power (at 5100A) we decompose the total infrared emission (L_IR; 8-1000um) into an AGN (L_IR,AGN) and star-forming component (L_IR,SF). We find that the AGN contribution to L_IR increases as a function of…
A Multiwavelength Inventory for the Local Group L-band Survey I: Atlas and Radial Profiles of Local Group Galaxies
National Radio Astronomy Observatory（国家射电天文台）；The Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astroparticle Physics (CCAPP)（宇宙学与亚原子物理中心）；University of Kentucky（肯塔基大学）；University of Alberta（阿尔伯塔大学）；University of Wisconsin–Madison（威斯康星大学麦迪逊分校）
