论文标题
大小 - 质量和其他结构参数（$ n，μ_z，r_z $），用于局部凸起/球体的关系多组分分解
The size--mass and other structural parameter ($n, μ_z, R_z$) relations for local bulges/spheroids from multicomponent decompositions
论文作者
论文摘要
我们分析了凸起/球体尺寸 - （恒星质量），$ r _ {\ rm e，sph} -m _ {\ rm *，sph} $，关系和连续性和球形结构参数，用于202本地（主要是$ \ simsim $ \ lyssim 110〜 \ \ rmMpc $）跨度$ mm m _ * 3 \ times10^{9} -10^{12}〜\ rm m _ {\ odot} $和$ 0.1 \ sillssim r _ {\ rm e，sph} \ sph} \ simeSim32〜 \ rm kpc kpc $ rm kpc $ kpc $ kpc $ kpc kpc $ kpc $ rom component ecomposition的分解。球体sérsic指数（$ n _ {\ rm sph} $），中央表面亮度（$μ_{\ rm 0，sph} $）之间的相关性，有效的半光半径（$ r _ {\ rm e，sph} $探索了恒星质量（$ m _ {\ rm *，sph} $）。我们还研究了使用不同比例半径的后果，$ r_ {z，\ rm sph} $，将总亮度的不同分数（$ z $，0到1）封装。预计质量密度的相关优势，$σ_z$和$ \langleσ\ rangle_z $，随着$ z $的选择而有很大差异。球体大小（$ r _ {\ rm z，sph} $）和质量（$ m _ {\ rm *，sph} $）在所有光分数$ z $上都密切相关。我们发现：$ \ log（r _ {\ rm e，sph}/\ rm kpc）= 0.88 \ log（m _ {\ rm *，sph}/\ rm m _ {\ odot}） - 9.15 $，带有$δ_{rms} = 0.24〜的少量散布，相对于\ textIt {弯曲}尺寸 - 质量的关系，讨论了该结果，因为它们的椎间盘在较低的质量下产生了较大的星系半径，因此对早期型星系的大小质量关系进行了讨论。此外，我们的球体尺寸质量关系的斜率为$ \ sim3 $，比报道的凸出尺寸质量关系陡峭，并且凸出尺寸为$ m _ {\ rm *，sph} \ sim 3 \ sim 3 \ times10^9〜m_ m_ \ odot $，是2至3倍。最后，我们表明本地球体与quiescent星系符合$ z \ sim1.25 $ - $ 2.25 $。从本质上讲，局部球体和高$ z $静态星系在结构上看起来很相似，这可能是病毒定理决定的。
We analyse the bulge/spheroid size-(stellar mass), $R_{\rm e,Sph}-M_{\rm *,Sph}$, relation and spheroid structural parameters for 202 local (predominantly $\lesssim 110~\rm Mpc$) galaxies spanning $ M_*\sim 3\times10^{9}-10^{12}~\rm M_{\odot}$ and $ 0.1 \lesssim R_{\rm e, Sph}\lesssim32~\rm kpc$ from multicomponent decomposition. The correlations between the spheroid Sérsic index ($n_{\rm Sph}$), central surface brightness ($μ_{\rm 0, Sph}$), effective half-light radius ($R_{\rm e, Sph}$), absolute magnitude ($\mathfrak{M}_{\rm Sph}$) and stellar mass ($M_{\rm *,Sph}$) are explored. We also investigate the consequences of using different scale radii, $R_{z,\rm Sph}$, encapsulating a different fraction ($z$, from 0 to 1) of the total luminosity. The correlation strengths for projected mass densities, $Σ_z$ and $\langle Σ\rangle_z$, vary significantly with the choice of $z$. Spheroid size ($R_{\rm z, Sph}$) and mass ($M_{\rm *,Sph}$) are strongly correlated for all light fractions $z$. We find: $\log(R_{\rm e,Sph}/\rm kpc) = 0.88\log(M_{\rm *,Sph}/\rm M_{\odot})-9.15$ with a small scatter of $Δ_{rms} = 0.24~\rm dex$. This result is discussed relative to the \textit{curved} size-mass relation for early-type galaxies due to their discs yielding larger galaxy radii at lower masses. Moreover, the slope of our spheroid size-mass relation is a factor of $\sim3$, steeper than reported bulge size-mass relations, and with bulge sizes at $M_{\rm *,sph}\sim 3\times10^9~M_\odot$ which are 2 to 3 times smaller. Finally, we show that the local spheroids align well with quiescent galaxies at $z\sim1.25$--$2.25$. In essence, local spheroids and high-$z$ quiescent galaxies appear structurally similar, likely dictated by the virial theorem.
