http://202.127.29.3/~shen/wiki/api.php?action=feedcontributions&feedformat=atom&user=ShenShiyin's note - 用户贡献 [zh-cn]2026-05-15T09:58:26Z用户贡献MediaWiki 1.38.1http://202.127.29.3/~shen/wiki/index.php?title=LAMOST&diff=4286LAMOST2026-04-29T03:26:20Z<p>Shen：创建页面，内容为“==LSF== * LAMOST 的线扩展函数 https://doi.org/10.3847/1538-3881/ae4ebe # Download and Install: git clone https://github.com/catty215/Construct_LAMOST_IP.git pip install -e . # Usage Example: from IP_construct import get_IP wl, flux = get_IP(spec_id, label1_time, label2_fiber, label3_line)”</p>
<hr />
<div>==LSF==<br />
* LAMOST 的线扩展函数 https://doi.org/10.3847/1538-3881/ae4ebe<br />
<br />
# Download and Install:<br />
git clone https://github.com/catty215/Construct_LAMOST_IP.git<br />
pip install -e .<br />
# Usage Example:<br />
from IP_construct import get_IP<br />
wl, flux = get_IP(spec_id, label1_time, label2_fiber, label3_line)</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E6%81%92%E6%98%9F%E5%BD%A2%E6%88%90%E6%95%88%E7%8E%87&diff=4285恒星形成效率2026-04-22T11:17:54Z<p>Shen：</p>
<hr />
<div>*https://arxiv.org/abs/2407.11125 常数？<br />
* https://arxiv.org/abs/2604.18504 支持全局的KS定理，与半径关系不大</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E6%81%92%E6%98%9F%E9%87%91%E5%B1%9E%E4%B8%B0%E5%BA%A6&diff=4284恒星金属丰度2026-04-22T11:07:30Z<p>Shen：</p>
<hr />
<div>==mass-metalicity relation==<br />
*arXiv 2208.06939: 局域恒星金属丰度与局域的势场强度相关（starforming和quenched星系都适用），这对星系的quench机制给出了约束，就是说大质量的qunech星系的金属丰度偏高，不大可能是仅仅因为化学演化上的starvation造成的（低丰度气体被剥离，恒星金属丰度会迅速上升），这样会导致要求星系的size也发生演化<br />
<br />
* 质量金属丰度关系：[Fe/H] = -2.6 - 0.075M_B，附近星系准确的测量 https://arxiv.org/abs/2604.18183</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%9B%BE%E5%83%8F%E5%A4%84%E7%90%86&diff=4283图像处理2026-04-22T00:44:10Z<p>Shen：</p>
<hr />
<div>[[PS图]]<br />
<br />
*格式转换<br />
ds9可以简单的完成图像格式的转换<br />
As an example, the following command will open the file "name.fits",<br />
zoom it to fit the window, save it in JPEG format to the file<br />
"filename.jpeg", and then exit<br />
ds9 name.fits -zoom to fit -saveimage jpeg filename.jpeg -exit<br />
ds9的command line 可以进行图像的批处理，具体可通过ds9 --help 查看。<br />
例如 ds9 -cmap heat a1.fits 可以用heat的颜色表来load图像。<br />
<br />
==图像的二阶距==<br />
*可以描述图像的椭率等参数，参见 [http://raphael.candelier.fr/?blog=Image%20Moments]<br />
<br />
==探测的完备性==<br />
* 用合成的源注入到巡天图像中，重新探测，来检查完备度，DES开发了一个软件Balrog [https://github.com/Kyle-Boone/ssi_corrections_des_y3_balrog]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E6%B0%94%E7%9B%B8%E9%87%91%E5%B1%9E%E4%B8%B0%E5%BA%A6&diff=4282气相金属丰度2026-04-21T13:40:29Z<p>Shen：/* 标定方法 */</p>
<hr />
<div>*AGN中的金属丰度 [https://arxiv.org/abs/1902.06368]arXiv:2309.05332<br />
:比相同质量的恒星形成星系要高，原因可能是因为吸积盘上的恒星形成，或者宽线区的尘埃被摧毁<br />
:金属丰度与星系的恒星质量相关性不强<br />
<br />
*气象金属丰度和[[恒星金属丰度]]的差异反映恒星形成历史<br />
:arXiv1905.04314:一些恒星形成区这两个金属丰度差不多<br />
<br />
<br />
==O丰度==<br />
*计算方法R23(Tremonti 2004)<br />
*Maiolino et al. (2008)<br />
<br />
===alpha元素===<br />
* 包括S,Ar,Ne等元素， S/O随着O丰度有变化，可能和S的部分SNIa起源有关系，另外O元素可能还有dust depeletion的效应 arXiv:2501.13586<br />
* To date, gas phase observations of sulphur in dense interstellar environments have only constrained the molecular carriers of 1% of its predicted cosmic abundance. An additional 5% is known to be locked up in molecular solids in dense clouds, leaving the main reservoir of depleted sulphur in the solid phase unknown. arXiv:2502.09384<br />
<br />
==N丰度==<br />
*CNO循环可以产生，在高金属丰度环境下，其产额与金属丰度有关<br />
*N元素在中等质量恒星中，产生和O元素（大质量恒星）的时标不太一样<br />
:star burst的星风可以吹走O，从而造成N/O偏高 （Van Zee & Haynes 2006）<br />
*因此，低金属丰度的时候N/O 常数，高丰度的时候N/O随着O/H增加而增加。<br />
<br />
<br />
==标定方法==<br />
*O3N2 (Marino et al. 2013)<br />
*ONS (Pilyugin et al. 2010)<br />
*不同标定方法之间的装换（用的MaNGA数据） arXiv:2108.04934<br />
*[[电子温度]]法，arXiv:2111.10748 <br />
:在MaNGA样本里面自己测量了OIII 4363，采用Te法测量了金属丰度，发现这些spaxel的区域在比较小质量星系中，这些小质量星系bias到merger样本。<br />
:这些可测量OIII 4363的spaxel星族年轻，恒星形成率高，但是金属丰度反常偏低anomalously low metallicity(ALM)（不能用FMR解释）<br />
*高红移：arXiv:2310.08622<br />
* DEep Spectra of Ionised REgions Database (DESIRED), the largest compilation of HII regions and galaxies with direct electron-temperature determinations [https://arxiv.org/abs/2604.16273]<br />
<br />
==科学结果==<br />
*Te方法直接探测到侧向旋涡星系气体内流（低金属丰度），外流（高金属丰度）[https://arxiv.org/abs/2108.13211]<br />
*利用两点相关函数的办法来探测空间分辨的金属丰度的涨落之间内在的关系[https://arxiv.org/abs/2206.08072]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Bar&diff=4281Bar2026-04-21T11:32:41Z<p>Shen：</p>
<hr />
<div>*描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498]<br />
<br />
==strength==<br />
The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).<br />
* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010)<br />
* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al. (2002); Marinova & Jogee (2007); Aguerri et al. (2009)<br />
* Fourier decomposition of the galaxy light Ohta et al. (1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).<br />
<br />
==pattern speed==<br />
defined as the rotational frequency of the bar. <br />
* Bar cannot extend beyond the corotation resonance (CR) radius of the galaxy.<br />
* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed. <br />
* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.<br />
* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054<br />
<br />
==形成机制==<br />
* Can A Kinematically Hot and Thick Disk Form A Bar? : Role of Highly Spinning Dark Matter Halos arXiv:2512.21632 <br />
:*高红移星系，动力学上更热，看到了棒结构，可能与旋转的晕有关。<br />
<br />
==star formation==<br />
* SFE 在棒上偏低 https://arxiv.org/abs/2604.15644</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E9%A6%96%E9%A1%B5&diff=4280首页2026-02-26T12:01:32Z<p>Shen：</p>
<hr />
<div>[[About Me]]<br />
<br />
<br />
==内容==<br />
[[天文]]<br />
<br />
[[计算机]]<br />
<br />
[[基础物理]]<br />
<br />
[[数理统计]]<br />
<br />
[[英语语法]]<br />
<br />
<br />
<br />
<br />
<br />
==帮助==<br />
*语法格式[http://www.mediawiki.org/w/index.php?title=Help:Formatting/zh&oldid=621228], 链接[http://www.mediawiki.org/wiki/Help:Links/zh], *图片[http://www.mediawiki.org/wiki/Help:Images/zh], *表格[http://www.mediawiki.org/wiki/Help:Tables/zh]<br />
*[[如何启用扩展]]，查看已经安装的扩展[[Special:Version]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E9%A6%96%E9%A1%B5&diff=4279首页2026-02-26T12:00:34Z<p>Shen：</p>
<hr />
<div>[[About Me]]<br />
<br />
我是沈世银<br />
<br />
==内容==<br />
[[天文]]<br />
<br />
[[计算机]]<br />
<br />
[[基础物理]]<br />
<br />
[[数理统计]]<br />
<br />
[[英语语法]]<br />
<br />
<br />
<br />
<br />
<br />
==帮助==<br />
*语法格式[http://www.mediawiki.org/w/index.php?title=Help:Formatting/zh&oldid=621228], 链接[http://www.mediawiki.org/wiki/Help:Links/zh], *图片[http://www.mediawiki.org/wiki/Help:Images/zh], *表格[http://www.mediawiki.org/wiki/Help:Tables/zh]<br />
*[[如何启用扩展]]，查看已经安装的扩展[[Special:Version]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Mediawiki&diff=4278Mediawiki2026-02-03T02:15:47Z<p>Shen：/* 备份 */</p>
<hr />
<div>==wiki架设==<br />
<br />
最近用mediawiki 配置了一个wiki网站给IFU项目使用。<br />
基本情况是需求以下服务：[[Apache]]+[[mysql]]+[[php]]<br />
<br />
<br />
===安装===<br />
*可以自己安装，但是需要较多的php包<br />
yum install -y httpd mysql-server php php-pear php-xml php-mysql php-intl php-pecl-apc php-gd php-mbstrin<br />
:安装之后重新启动httpd服务<br />
:如果报错，注意检查http的错误log，在/var/log/httpd/error_log<br />
<br />
;mediawiki的安装界面比较友好。安装好之后要将[[Apache]]服务配置好。<br />
<br />
;需要创建一个[[mysql]]的数据库<br />
<br />
;Wiki的配置最重要要是更改 LocalSettings.php 文件<br />
<br />
*有不需要数据库服务的wiki，可以U盘带走，这个比较好。具体参考http://www.mediawiki.org/wiki/Manual:Wiki_on_a_stick<br />
<br />
*可以用系统自带的rpm包，fc下，直接把/usr/share/mediawiki/目录下的文件复制到你要的目录就可以了（在1.32之前，符号链接都可，1.32不知道为什么不可以了）<br />
<br />
===[[SELinux]]===<br />
这个比较烦人，参考https://www.mediawiki.org/wiki/SELinux<br />
<br />
<br />
==配置==<br />
*对没有登录的 用户移除页面顶部的讨论页链接在LocalSetting.php里添加<br />
$wgShowIPinHeader = false;<br />
<br />
===用户权限===<br />
*以下内容设置匿名用户可浏览，注册，但不能编辑。注册用户可编辑<br />
$wgGroupPermissions['*' ]['createaccount'] = true;<br />
$wgGroupPermissions['*' ]['read'] = true;<br />
$wgGroupPermissions['*' ]['edit'] = false;<br />
$wgGroupPermissions['user' ]['createaccount'] = true;<br />
$wgGroupPermissions['user' ]['edit'] = true;<br />
<br />
*阻止新用户注册 <br />
$wgGroupPermissions['*' ]['createaccount'] = false;<br />
;注 意：阻止新用户注册，此时管理员可以到特殊页面上的用户登录页面（Special<nowiki>:</nowiki>UserLogin）里，输入希望为其建立帐户的某人的用户名与电子邮 件地址，然后点击通过eMail（by email）按钮递交，系统将创建帐号并将随机生成的密码发送到指定email里。<br />
<br />
*设置匿名用户可读内容<br />
$wgWhitelistRead = array( "Main Page", "Special:Userlogin" );<br />
$wgGroupPermissions['*' ]['read'] = false;<br />
;注 意：具体需要对应自己的站点链接，而对于多字节语言的MediaWiki，例如中文首页链接index.php?title=%E9%A6%96%E9 %A1%B5，这首页中文字符PHP可能无法正确解码。需要利用urldecode()函数转换一下，写为：$wgWhitelistRead = array( urldecode("%E9%A6%96%E9%A1%B5") ;<br />
<br />
===文件上传===<br />
*配置文件上传，修改如下内容<br />
## To enable image uploads, make sure the 'images' directory<br />
## is writable, then set this to true:<br />
$wgEnableUploads = true;<br />
#$wgUploadPath = "$IP/img_auth.php"; <br />
#$wgUploadDirectory = "$IP/images"; #默认值，这个文件夹应该有写入权限 （我设置了777不知道对不对）<br />
$wgFileExtensions =array('png','gif','jpg','jpeg','doc','xls','mpp','pdf','ppt','tiff','bmp','docx','xlsx','pptx','ps','odt','ods','odp','odg'); ＃文件扩展名限制，不知道是否可以设置任意文件类型，还有文件大小限制默认的是2M，如何设置？(这个好像是[[php]]的限制）<br />
<br />
注意<br />
#$wgUploadPath = "$IP/img_auth.php"; <br />
#$wgUploadDirectory = "$IP/images"; <br />
以上两句是不需要的，我在1.23.8里面设置之后反而出错。<br />
<br />
:一种原因是因为SELinux<br />
sudo chcon -R -t httpd_sys_content_rw_t images （ 这个重新启动后可能会失效）<br />
:另外注意检查images目录下是否有.htaccess文件，注意设置images目录的权限<br />
chown apache -R images<br />
chgrp apache -R images<br />
chmod 755 -R images<br />
<br />
*无法创建目录“mwstore://local-backend/local-public/c/ca”错误<br />
sudo chown -R www-data:www-data images/ <br />
<br />
<br />
*文件大小限制<br />
修改/etc/php/php.ini的两个配置项<br />
post_max_size<br />
upload_max_filesize<br />
注意重新启动httpd使设置生效。在fc35中，还需要重启php-fpm服务。<br />
<br />
*不能上传script文件，出现警告：有可能引起浏览器错误<br />
$wgDisableUploadScriptChecks = true;<br />
<br />
*新版本的wiki还要对文件的格式做事实上的检查，可以通过下面的设置关掉<br />
$wgCheckFileExtensions = false;<br />
$wgStrictFileExtensions = false;<br />
这两个配置不一定在Localsetting里面，而是在includes/DefaultSetting这个文件中间<br />
<br />
===无法显示缩略图===<br />
*出错信息libgomp: Thread creation failed: Resource temporarily unavailable<br />
$wgMaxShellMemory = 406900 ；<br />
<br />
==使用==<br />
[[wiki语法]]<br />
<br />
===扩展===<br />
*[[如何启用扩展]]<br />
*自带的扩展启用后，可以通过[[Special:Version]]查看<br />
*搜索，下载 [http://www.mediawiki.org/wiki/Special:ExtensionDistributor]<br />
*下面是我自己下载的两个，感觉比较有用的扩展(mediawiki 1.38)<br />
<br />
====Lockdown====<br />
*实现某些页面只有登录用户才能阅读的功能，参见[https://www.mediawiki.org/wiki/Extension:Lockdown]<br />
*这些页面要用namespace来特殊定义，比如[http://cluster.shao.ac.cn/wiki/index.php/Internal:Iserver]<br />
wfLoadExtension( 'Lockdown' )<br />
#define custom namespaces<br />
$wgExtraNamespaces[100] = "Internal";<br />
#restrict "read" permission to logged in users<br />
$wgNamespacePermissionLockdown[100]['read'] = array('user');<br />
<br />
====ConfirmAccount====<br />
*实现需审核（邮件通知）的自助注册<br />
<br />
====SwiftMailer====<br />
*设置wiki的邮件系统，<br />
:*Localsettings中设置 <br />
$wgEnableEmail = true;<br />
:*科学院邮件需要编辑 "extension.json" file:<br />
<br />
"config": {<br />
"SMTPAuthenticationMethod": {<br />
"value": "ssl" <br />
}<br />
},<br />
<br />
<br />
===管理===<br />
*忘记用户密码<br />
php maintenance/changePassword.php --user=username --password=newpassword<br />
<br />
*无法显示<br />
查看httpd状态，一堆报错，<br />
SELinux is preventing /usr/sbin/httpd from getattr access on the file <br />
解决方法<br />
restorecon -v -R /opt/www/<br />
<br />
===备份===<br />
*单个页面导出[[Special:Export]],页面导入[[Special:Import]]<br />
*完整备份为xml文件 <br />
php maintenance/dumpBackup.php --full --conf LocalSettings.php > dump.xml<br />
*xml的备份，可以用wikiTaxi软件打开<br />
*mysql的数据库备份<br />
mysqldump -u root -p*** wikidb | gzip > /bak/wikidb.bakup.gz<br />
*整个wikipedia的备份可以参见 [https://meta.wikimedia.org/wiki/Data_dump_torrents]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Mediawiki&diff=4277Mediawiki2026-02-03T00:53:32Z<p>Shen：</p>
<hr />
<div>==wiki架设==<br />
<br />
最近用mediawiki 配置了一个wiki网站给IFU项目使用。<br />
基本情况是需求以下服务：[[Apache]]+[[mysql]]+[[php]]<br />
<br />
<br />
===安装===<br />
*可以自己安装，但是需要较多的php包<br />
yum install -y httpd mysql-server php php-pear php-xml php-mysql php-intl php-pecl-apc php-gd php-mbstrin<br />
:安装之后重新启动httpd服务<br />
:如果报错，注意检查http的错误log，在/var/log/httpd/error_log<br />
<br />
;mediawiki的安装界面比较友好。安装好之后要将[[Apache]]服务配置好。<br />
<br />
;需要创建一个[[mysql]]的数据库<br />
<br />
;Wiki的配置最重要要是更改 LocalSettings.php 文件<br />
<br />
*有不需要数据库服务的wiki，可以U盘带走，这个比较好。具体参考http://www.mediawiki.org/wiki/Manual:Wiki_on_a_stick<br />
<br />
*可以用系统自带的rpm包，fc下，直接把/usr/share/mediawiki/目录下的文件复制到你要的目录就可以了（在1.32之前，符号链接都可，1.32不知道为什么不可以了）<br />
<br />
===[[SELinux]]===<br />
这个比较烦人，参考https://www.mediawiki.org/wiki/SELinux<br />
<br />
<br />
==配置==<br />
*对没有登录的 用户移除页面顶部的讨论页链接在LocalSetting.php里添加<br />
$wgShowIPinHeader = false;<br />
<br />
===用户权限===<br />
*以下内容设置匿名用户可浏览，注册，但不能编辑。注册用户可编辑<br />
$wgGroupPermissions['*' ]['createaccount'] = true;<br />
$wgGroupPermissions['*' ]['read'] = true;<br />
$wgGroupPermissions['*' ]['edit'] = false;<br />
$wgGroupPermissions['user' ]['createaccount'] = true;<br />
$wgGroupPermissions['user' ]['edit'] = true;<br />
<br />
*阻止新用户注册 <br />
$wgGroupPermissions['*' ]['createaccount'] = false;<br />
;注 意：阻止新用户注册，此时管理员可以到特殊页面上的用户登录页面（Special<nowiki>:</nowiki>UserLogin）里，输入希望为其建立帐户的某人的用户名与电子邮 件地址，然后点击通过eMail（by email）按钮递交，系统将创建帐号并将随机生成的密码发送到指定email里。<br />
<br />
*设置匿名用户可读内容<br />
$wgWhitelistRead = array( "Main Page", "Special:Userlogin" );<br />
$wgGroupPermissions['*' ]['read'] = false;<br />
;注 意：具体需要对应自己的站点链接，而对于多字节语言的MediaWiki，例如中文首页链接index.php?title=%E9%A6%96%E9 %A1%B5，这首页中文字符PHP可能无法正确解码。需要利用urldecode()函数转换一下，写为：$wgWhitelistRead = array( urldecode("%E9%A6%96%E9%A1%B5") ;<br />
<br />
===文件上传===<br />
*配置文件上传，修改如下内容<br />
## To enable image uploads, make sure the 'images' directory<br />
## is writable, then set this to true:<br />
$wgEnableUploads = true;<br />
#$wgUploadPath = "$IP/img_auth.php"; <br />
#$wgUploadDirectory = "$IP/images"; #默认值，这个文件夹应该有写入权限 （我设置了777不知道对不对）<br />
$wgFileExtensions =array('png','gif','jpg','jpeg','doc','xls','mpp','pdf','ppt','tiff','bmp','docx','xlsx','pptx','ps','odt','ods','odp','odg'); ＃文件扩展名限制，不知道是否可以设置任意文件类型，还有文件大小限制默认的是2M，如何设置？(这个好像是[[php]]的限制）<br />
<br />
注意<br />
#$wgUploadPath = "$IP/img_auth.php"; <br />
#$wgUploadDirectory = "$IP/images"; <br />
以上两句是不需要的，我在1.23.8里面设置之后反而出错。<br />
<br />
:一种原因是因为SELinux<br />
sudo chcon -R -t httpd_sys_content_rw_t images （ 这个重新启动后可能会失效）<br />
:另外注意检查images目录下是否有.htaccess文件，注意设置images目录的权限<br />
chown apache -R images<br />
chgrp apache -R images<br />
chmod 755 -R images<br />
<br />
*无法创建目录“mwstore://local-backend/local-public/c/ca”错误<br />
sudo chown -R www-data:www-data images/ <br />
<br />
<br />
*文件大小限制<br />
修改/etc/php/php.ini的两个配置项<br />
post_max_size<br />
upload_max_filesize<br />
注意重新启动httpd使设置生效。在fc35中，还需要重启php-fpm服务。<br />
<br />
*不能上传script文件，出现警告：有可能引起浏览器错误<br />
$wgDisableUploadScriptChecks = true;<br />
<br />
*新版本的wiki还要对文件的格式做事实上的检查，可以通过下面的设置关掉<br />
$wgCheckFileExtensions = false;<br />
$wgStrictFileExtensions = false;<br />
这两个配置不一定在Localsetting里面，而是在includes/DefaultSetting这个文件中间<br />
<br />
===无法显示缩略图===<br />
*出错信息libgomp: Thread creation failed: Resource temporarily unavailable<br />
$wgMaxShellMemory = 406900 ；<br />
<br />
==使用==<br />
[[wiki语法]]<br />
<br />
===扩展===<br />
*[[如何启用扩展]]<br />
*自带的扩展启用后，可以通过[[Special:Version]]查看<br />
*搜索，下载 [http://www.mediawiki.org/wiki/Special:ExtensionDistributor]<br />
*下面是我自己下载的两个，感觉比较有用的扩展(mediawiki 1.38)<br />
<br />
====Lockdown====<br />
*实现某些页面只有登录用户才能阅读的功能，参见[https://www.mediawiki.org/wiki/Extension:Lockdown]<br />
*这些页面要用namespace来特殊定义，比如[http://cluster.shao.ac.cn/wiki/index.php/Internal:Iserver]<br />
wfLoadExtension( 'Lockdown' )<br />
#define custom namespaces<br />
$wgExtraNamespaces[100] = "Internal";<br />
#restrict "read" permission to logged in users<br />
$wgNamespacePermissionLockdown[100]['read'] = array('user');<br />
<br />
====ConfirmAccount====<br />
*实现需审核（邮件通知）的自助注册<br />
<br />
====SwiftMailer====<br />
*设置wiki的邮件系统，<br />
:*Localsettings中设置 <br />
$wgEnableEmail = true;<br />
:*科学院邮件需要编辑 "extension.json" file:<br />
<br />
"config": {<br />
"SMTPAuthenticationMethod": {<br />
"value": "ssl" <br />
}<br />
},<br />
<br />
<br />
===管理===<br />
*忘记用户密码<br />
php maintenance/changePassword.php --user=username --password=newpassword<br />
<br />
*无法显示<br />
查看httpd状态，一堆报错，<br />
SELinux is preventing /usr/sbin/httpd from getattr access on the file <br />
解决方法<br />
restorecon -v -R /opt/www/<br />
<br />
===备份===<br />
*单个页面导出[[Special:Export]],页面导入[[Special:Import]]<br />
*完整备份为xml文件 <br />
php maintenance/dumpBackup.php --full --conf LocalSettings.php > dump.xml<br />
*xml的备份，可以用wikiTaxi软件打开<br />
*mysql的数据库备份<br />
mysqldump -u root -p751006abc wikidb | gzip > /bak/wikidb.bakup.gz<br />
*整个wikipedia的备份可以参见 [https://meta.wikimedia.org/wiki/Data_dump_torrents]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=SPHEREx&diff=4276SPHEREx2026-01-30T11:08:45Z<p>Shen：创建页面，内容为“*SPHEREx is based on a telescope with an effective 20 cm diameter and a 11°x3.5° field of view. *SPHEREx will obtain near-infrared 0.75-5.0 µm spectra every 6" over the entire sky. *窄带测光 R = 35-130”</p>
<hr />
<div>*SPHEREx is based on a telescope with an effective 20 cm diameter and a 11°x3.5° field of view.<br />
*SPHEREx will obtain near-infrared 0.75-5.0 µm spectra every 6" over the entire sky.<br />
*窄带测光 R = 35-130</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E6%98%9F%E6%97%8F%E5%90%88%E6%88%90&diff=4275星族合成2026-01-29T09:29:28Z<p>Shen：/* alf */</p>
<hr />
<div>*[[近红外谱]]的合成与光学谱的结果的比较 arXiv.1802.08280<br />
:对谱的分辨率较敏感，敏感于TP-AGB星，不同的libaray有差别<br />
<br />
http://www.sedfitting.org/<br />
==SSP==<br />
*PEGASE：考虑了金属丰度的自演化和尘埃？<br />
<br />
==常用的CODE==<br />
*卢家风开发了一种不依赖于尘埃减光的星族合成方法ewsps（参考ppxf）<br />
*不同SSP模版的比较 https://arxiv.org/pdf/2506.02099 （消光曲线的重要性）<br />
===MAGPHYS===<br />
*robust statistical constraints on key parameters describing the stellar content,star formation activity,dust content of galaxies. <br />
*publicly available via a user-friendly code package, MAGPHYS at www.iap.fr/magphys<br />
*GPU加速 （Chang Hee Ree)<br />
<br />
===FSPS===<br />
*Flexible Stellar Population Synthesis<br />
*有[[IDL]]的读写程序<br />
*https://github.com/cconroy20/fsps<br />
<br />
===starburst99===<br />
*有远紫外的光谱，发射线模板<br />
<br />
===PROSPECT===<br />
*[https://github.com/asgr/ProSpect]<br />
*http://prospect.icrar.org<br />
*考虑了简单的化学演化（close-box）<br />
*AGN模板<br />
*尘埃：能量平衡，年轻星族消光，年老星族消光，AGN消光<br />
*发射线：短于912A的光子，部分被吸收，再以发射线形式出来（能量平衡）<br />
*可以生成SED，应用在SAM上，也可以用MCMC来做参数拟合<br />
<br />
===DSPS===<br />
*将星族合成中的常用过程都做了可以微分化的处理，这样在做优化工作的时候可以利用梯度下降进行，因此可以大大提高速度。<br />
*文章：arXiv:2112.06830，CODE： [https://github.com/ArgonneCPAC/dsps]<br />
<br />
===pyparadise===<br />
*这个拟合方法是把光谱先拉平 [https://github.com/brandherd/PyParadise/]<br />
===galapy===<br />
* [https://galapy.readthedocs.io/en/latest/general/install_guide.html] 全新的python工具，用的c++库，有尘埃模型<br />
<br />
==不常用的==<br />
===alf===<br />
*全谱拟合，主要是对老年星系，探讨不同的元素比例对吸收线的贡献 （arXiv:1901.06391）<br />
*貌似能够更好的拟合老年星系的宽波段颜色<br />
* 可以讨论采用不同的IMF （https://arxiv.org/pdf/2601.20864）<br />
<br />
===SNITCH===<br />
*参数化的恒星形成历史，不考虑化学演化，拟合几个谱线特征 arXiv 1901.07036<br />
*MCMC 跑，精修Chain （把概率小的地方修掉）什么鬼！<br />
<br />
==推论==<br />
*不同方法（信噪比下）得到的年龄分辨率到底能到多少？（2401.07335）<br />
<br />
==其它==<br />
<br />
<br />
==isochrone==<br />
*BaSTI [http://albione.oa-teramo.inaf.it/]<br />
<br />
---<br />
*带发射线的SED拟合，参见http://arxiv.org/abs/1509.05055<br />
---<br />
*[[BC03]]<br />
*CIGALE<br />
:Code Investigating Galaxy Emission</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pytorch&diff=4274Pytorch2026-01-29T07:05:59Z<p>Shen：/* cuda */</p>
<hr />
<div>*英文文档：[https://pytorch.org/docs/stable/index.html]<br />
*中文文档 [https://pytorch.apachecn.org/][https://pytorch-cn.readthedocs.io/zh/latest/package_references/functional/#convolution]<br />
==cuda==<br />
*torch.cuda.is_available()<br />
*torch.version.cuda() #查看cuda版本<br />
*torch.backends.cudnn.version #查看cudnn版本<br />
*nvcc -V 查看cuda版本号<br />
*nvidia-smi 查看程序运行情况<br />
* cudnn安装 https://zhuanlan.zhihu.com/p/691711768<br />
<br />
<br />
===查看显卡信息===<br />
*查看当前设备环境可用显卡数量, 及可用显卡的具体信息（型号、算力，显存以及线程数）<br />
ng = torch.cuda.device_count()<br />
infos = [torch.cuda.get_device_properties(i) for i in range(ng)]<br />
<br />
===指定显卡===<br />
* 代码1： torch.cuda.set_device(1)<br />
* 代码2：device = torch.device("cuda:1")<br />
* 代码3：（官方推荐使用）：os.environ["CUDA_VISIBLE_DEVICES"] = '1'<br />
*（如果你想同时调用两块GPU的话）： os.environ["CUDA_VISIBLE_DEVICES"] = '1,2'<br />
<br />
==网络初始化==<br />
*Xavier and Kaiming initialization [https://www.jianshu.com/p/f2d800388d1c]<br />
<br />
==数据准备==<br />
import torch<br />
import torch.utils.data as Data<br />
torch.manual_seed(1) # reproducible<br />
BATCH_SIZE = 5 # 批训练的数据个数<br />
x = torch.linspace(1, 10, 10) # x data (torch tensor)<br />
y = np.arange(1, 10)<br />
y = torch.from_numpy(y) #numpy ndarray to torch tensor <br />
torch_dataset = Data.TensorDataset(x, y) # 换成 torch 能识别的 Dataset<br />
# 把 dataset 放入 DataLoader<br />
loader = Data.DataLoader(<br />
dataset=torch_dataset, # torch TensorDataset format<br />
batch_size=BATCH_SIZE, # mini batch size<br />
shuffle=True, # 要不要打乱数据 (打乱比较好)<br />
num_workers=2, # 多线程来读数据<br />
sampler=tr_sampler, #<br />
)<br />
<br />
<br />
===nan问题===<br />
*第一个是判断条件，第二个是符合条件的设置值，第三个是不符合条件的设置值。<br />
a = torch.Tensor([[1, 2, np.nan], [2, np.nan, 4], [3, 4, 5]])<br />
a = torch.where(torch.isnan(a), torch.full_like(a, 0), a)<br />
<br />
===数据初值归一化===<br />
*from sklearn.preprocessing import scale<br />
:其中scale可以对一维数据标准化（自动或略nan）<br />
*from sklearn.preprocessing import StandardScaler<br />
:StandardScaler是个类，默认对二维数据进行归一化，先fit再transform（类的方法），也可以fit_transform一起做，关键是后面可以inverse_transform()再把数据变回去。<br />
<br />
==Tensor==<br />
* 获取 Tensor 的元素个数 ，a.numel() 等价 a.nelement()<br />
* 查看 Tensor 的形状，Tensor.size() 返回 torch.Size() 对象， Tensor.shape 等价于 Tensor.size()<br />
* 通过 tensor.view 方法可以调整 tensor 的形状，但必须保证调整前后的元素总数保持一致，view 不会修改自身的数据，返回的新 tensor 与源 tensor 共享内存，即更改其中一个，另外一个也跟着改变。<br />
* 添加或减少某一维度，可以使用 squeeze 和 unsqueeze 函数。<br />
:*squeeze()删除一个张量中所有维数为1的维度<br />
* resize 是另一种可用来调整 size 的方法，但与 view 不同，它可以修改 tensor 的尺寸，如果新尺寸超过了源尺寸，会自动分配新的内存空间，而如果新尺寸小于源尺寸，则之前的数据依旧会被保存。<br />
* cpu() numpy()<br />
res=scores.cpu().numpy()<br />
:注意cuda上面的变量类型只能是tensor，不能是其他,把一个GPU上出来的数据转换成numpy ndarry<br />
* detach() item() [https://blog.csdn.net/ODIMAYA/article/details/102892799]<br />
<br />
<br />
==torchvision==<br />
*PyTorch框架中有一个非常重要且好用的包：torchvision，该包主要由3个子包组成，分别是：torchvision.datasets、torchvision.models、torchvision.transforms [https://www.jianshu.com/p/1ae863c1e66d]<br />
*__all__ = ["Compose", "ToTensor", "ToPILImage", "Normalize", "Resize",<br />
"Scale", "CenterCrop", "Pad", "Lambda", "RandomCrop", <br />
"RandomHorizontalFlip", "RandomVerticalFlip", "RandomResizedCrop", <br />
"RandomSizedCrop", "FiveCrop", "TenCrop","LinearTransformation", <br />
"ColorJitter", "RandomRotation", "Grayscale", "RandomGrayscale"]<br />
<br />
<br />
==函数==<br />
*torch.clamp(input, min=None, max=None, *, out=None) → Tensor<br />
:Clamps all elements in input into the range [ min, max ]. Letting min_value and max_value be min and max, respectively<br />
*torch.eye(n, m=None, out=None)<br />
:返回一个2维张量，对角线位置全1，其它位置全0<br />
*torch.cat & torch.stack<br />
:torch.stack()沿着一个新维度对输入张量序列进行连接。 序列中所有的张量都应该为相同形状。<br />
:torch.cat()是为了把函数torch.stack()得到tensor进行拼接而存在的 (不增加新的维度)<br />
*gather<br />
:In PyTorch you can perform the same operation using the gather() method. If s is a PyTorch Tensor of shape (N, C) and y is a PyTorch Tensor of shape (N,) containing longs in the range 0 <= y[i] < C, then s.gather(1, y.view(-1, 1)).squeeze() will be a PyTorch Tensor of shape (N,) containing one entry from each row of s, selected according to the indices in y.<br />
<br />
==第三方库==<br />
*thop<br />
:THOP 是 PyTorch 非常实用的一个第三方库，可以统计模型的 FLOPs 和参数量。<br />
from thop import clever_format<br />
from thop import profile<br />
class YourModule(nn.Module):<br />
# your definition<br />
input = torch.randn(10, 128, 128)<br />
flops, params = profile(model, inputs=(input, ))<br />
flops, params = clever_format([flops, params], "%.3f")</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=LRD&diff=4273LRD2026-01-29T03:11:46Z<p>Shen：</p>
<hr />
<div>little red dot <br />
# JWST上天后高红移宇宙最有意思的发现之一<br />
<br />
==观测特征==<br />
* compact morphology： majority of LRDs are not hosted by well-established, massive galaxies; instead, their nuclear BHs appear to be overmassive relative to the local BH-to-galaxy mass correlation,<br />
*UV-optical spectral energy distributions (SEDs) with a turnover wavelength around rest-frame ≃ 4000 ̊A, their broad-line emission properties, and the weakness in canonical AGN signatures such as hot dust and X-ray corona emission.<br />
*However, deep JWST/MIRI and ALMA observations show no significant detection of reprocessed IR flux in LRDs<br />
*To date, the JWST observational programs have not been originally designed for multi-epoch observations and make the detection of variability challenging.<br />
<br />
==模型==<br />
* A red optical from dust reddened, obscured AGNs and a blue UV excess from scattered light (dust and electrons) leaking through a patchy, partially covering medium.<br />
* 气体吸收可以解释balmer break和Balmer吸收 arXiv:2512.03130<br />
* 致宽不是运动学致宽，是电子散射 arXiv:2601.18864 （exponential form of the broad line wings）<br />
:* Sirocco selfconsistently computes the cocoon’s ionisation structure and radiation field(57),</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=LRD&diff=4272LRD2026-01-29T01:54:25Z<p>Shen：创建页面，内容为“little red dot # JWST上天后高红移宇宙最有意思的发现之一 ==观测特征== * compact morphology： majority of LRDs are not hosted by well-established, massive galaxies; instead, their nuclear BHs appear to be overmassive relative to the local BH-to-galaxy mass correlation, *UV-optical spectral energy distributions (SEDs) with a turnover wavelength around rest-frame ≃ 4000 ̊A, their broad-line emission properties, and the weakness in canoni…”</p>
<hr />
<div>little red dot <br />
# JWST上天后高红移宇宙最有意思的发现之一<br />
<br />
==观测特征==<br />
* compact morphology： majority of LRDs are not hosted by well-established, massive galaxies; instead, their nuclear BHs appear to be overmassive relative to the local BH-to-galaxy mass correlation,<br />
*UV-optical spectral energy distributions (SEDs) with a turnover wavelength around rest-frame ≃ 4000 ̊A, their broad-line emission properties, and the weakness in canonical AGN signatures such as hot dust and X-ray corona emission.<br />
*However, deep JWST/MIRI and ALMA observations show no significant detection of reprocessed IR flux in LRDs<br />
*To date, the JWST observational programs have not been originally designed for multi-epoch observations and make the detection of variability challenging.<br />
<br />
==模型==<br />
* A red optical from dust reddened, obscured AGNs and a blue UV excess from scattered light (dust and electrons) leaking through a patchy, partially covering medium.<br />
* 气体吸收可以解释balmer break和Balmer吸收 arXiv:2512.03130<br />
* 致宽不是运动学致宽，是电子散射 arXiv:2601.18864 （exponential form of the broad line wings）</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Diffuse_ionized_gas&diff=4271Diffuse ionized gas2026-01-29T01:07:51Z<p>Shen：</p>
<hr />
<div>[[electron temperature|电子温度]]<br />
<br />
==[[IFS观测]]==<br />
*DIG可以用Ha的等值宽度来做判据，EW(Ha)双峰分布<br />
*arXiv1907.08635：讨论了DIG对金属丰度测量的影响<br />
<br />
==银河系中的DIG==<br />
*Referred to as the Reynolds layer, or warm ionized medium (WIM); <br />
*This warm (10^4 K), diffuse (n ~ 0.2 cm~3) gas fills 20% of the disk volume and accounts for most of the mass of ionized gas(90 percent).<br />
:*[[电子密度]]比 hot gas要高一点（ Typical values of the central electron density, central cooling time and total mass for the ETGs are ~ 0.1cm−3, ~ 5 x 10^6 yr and 5 x 1O^9 M⊙）<br />
*In terms of energetics, the Galactic WIM requires at least 10^42 ergs s~1 to remain ionized. This power is more than can be comfortably supplied by supernova shocks, but significantly less than the [[Lyman continuum]] luminosity of massive stars.<br />
*[http://iopscience.iop.org/article/10.1086/306232/meta]<br />
<br />
==DIG对观测量的影响==<br />
* https://arxiv.org/abs/2601.19725v1 DIG区域，电离参数更小，金属丰度“更高”（不一定真实，从强线calibrator得到的结果）</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pixi&diff=4270Pixi2026-01-24T09:24:19Z<p>Shen：</p>
<hr />
<div>*一个替代conda的环境软件管理工具, <br />
* vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"<br />
*[autogalaxy]的安装指定 2024.11.6.1能避免很多兼容问题<br />
* pixi add torch==2.0</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Jax&diff=4269Jax2026-01-24T09:23:37Z<p>Shen：</p>
<hr />
<div>*简单的说就是GPU加速、支持自动微分(autodiff)的numpy。参考[https://jax.readthedocs.io/en/latest/notebooks/quickstart.html]<br />
*[https://cloud.tencent.com/developer/article/1593308]<br />
<br />
==安装==<br />
*jax和jaxlib版本要匹配（注意cuda支持）<br />
*我的CUDA版本是11.1 ，卡是A40，系统是[[Ubuntu]]，cudnn版本是805<br />
*安装最新版本 jax 0.2.26和jaxlib0.1.75后会在random函数报错“CustomCall failed: jaxlib/cuda_prng_kernels.cc:30: operation cudaGetLastError() failed: the provided PTX was compiled with an unsupported toolchain”<br />
:*最后安装的 jax0.2.2 (pip install -v jax==0.2.2), jaxlib是0.1.72 [https://storage.googleapis.com/jax-releases/cuda111/jaxlib-0.1.72+cuda111-cp38-none-manylinux2010_x86_64.whl]解决问题<br />
:*好像是因为一定要11.1的驱动11的不行（或者cudnn的问题）<br />
* 2026/01/24: 安装 jaxjaxlib-0.4.13+cuda11.cudnn86-cp311-cp311-manylinux2014_x86_64.whl 成功</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pixi&diff=4268Pixi2026-01-24T09:18:55Z<p>Shen：</p>
<hr />
<div>*一个替代conda的环境软件管理工具, <br />
* vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"<br />
*[autogalaxy]的安装指定 2024.11.6.1能避免很多兼容问题<br />
* 要让Nserver上的cuda，需要安装jaxjaxlib-0.4.13+cuda11.cudnn86-cp311-cp311-manylinux2014_x86_64.whl <br />
:* torch==2.0</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pixi&diff=4267Pixi2026-01-24T09:02:19Z<p>Shen：</p>
<hr />
<div>*一个替代conda的环境软件管理工具, <br />
* vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"<br />
*[autogalaxy]的安装指定 2024.11.6.1能避免很多兼容问题<br />
* 要让Nserver上的cuda，需要安装jaxjaxlib-0.4.13+cuda11.cudnn86-cp311-cp311-manylinux2014_x86_64.whl</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pixi&diff=4266Pixi2026-01-24T07:32:20Z<p>Shen：</p>
<hr />
<div>*一个替代conda的环境软件管理工具<br />
* vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"<br />
*[autogalaxy]的安装指定 2024.11.6.1能避免很多兼容问题</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Pixi&diff=4265Pixi2026-01-23T02:45:27Z<p>Shen：创建页面，内容为“*一个替代conda的环境软件管理工具 * vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"”</p>
<hr />
<div>*一个替代conda的环境软件管理工具<br />
* vscode中使用kernel python -m ipykernel install --user --name myenv --display-name "Python (myenv)"</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=BPT_diagram&diff=4264BPT diagram2026-01-22T11:06:25Z<p>Shen：</p>
<hr />
<div>*OIII/Hbeta VS NII/Halpha<br />
:不一定4条线都有才能区分，3条加一个upper limit也可以<br />
:通常 OIII和Hbeta比较弱，更难探测，主要是一些弱的AGN或者金属丰度比较高的恒星形成星系。<br />
:大质量星系容易出现Hbeta强，OIII，低金属丰度容易Halpha强，NII弱；<br />
:有一些星系没有巴尔沫线，但是有OIII和NII，（高电离态）<br />
<br />
*有一个类似的图用<nowiki>[SII]λ6717</nowiki>+6713/Halpha 代替NII/Halpha，成为VO87<br />
:该图能区分[[LINER]]和AGN，BPT不能<br />
<br />
*OIII/Hbeta 可能不完全能表征AGN<br />
:Maragkoudakis et al. (2014) revealed that galaxies with extranuclear star formation can show higher [O III] λ5007/Hβ line ratios, since lower metallicity H II regions in the outer parts of galaxy discs are also capable of producing high-excitation emis- sion lines.<br />
<br />
*高红移和低红移有一些系统的shift<br />
:In order to explain offsets between z ∼ 0 and high- redshift galaxies in diagnostic plots such as the [O iii]/Hβ vs. [N ii]/Hα diagram, it has been proposed that high-redshift galaxies may have higher ionization parameters (Kewley et al. 2015; Cullen et al. 2016), harder ionizing stellar spectra (Steidel et al. 2014), higher density/ISM pressure (Kewley et al. 2013; Sanders et al. 2016), and/or anomalous nitrogen abundance at fixed O/H (Masters 2 Sanders et al. et al. 2014; Shapley et al. 2015; Sanders et al. 2016) compared to z ∼ 0 galaxies. Depending<br />
<br />
* arXiv:2601.14542 用这个图来做AGN和恒星成分的分解</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Nuclear_ring&diff=4263Nuclear ring2026-01-19T08:30:08Z<p>Shen：创建页面，内容为“* AINUR: Atlas of Images of NUclear Rings * arXiv:2601.11127 Molecular gas and star formation in central rings across nearby galaxies * 银河系中间有个Central Molecular Zone，应该也是这个结构”</p>
<hr />
<div>* AINUR: Atlas of Images of NUclear Rings<br />
* arXiv:2601.11127 Molecular gas and star formation in central rings across nearby galaxies<br />
* 银河系中间有个Central Molecular Zone，应该也是这个结构</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E9%AB%98%E7%BA%A2%E7%A7%BB%E6%98%9F%E7%B3%BB&diff=4262高红移星系2026-01-19T08:28:02Z<p>Shen：创建页面，内容为“* arXiv:2601.11515 一个红移 z=13.53的星系PAN-z14-1，红移第4高，发射线不是很强，比较正常尺寸，和GS-z14-0比较相似”</p>
<hr />
<div>* arXiv:2601.11515 一个红移 z=13.53的星系PAN-z14-1，红移第4高，发射线不是很强，比较正常尺寸，和GS-z14-0比较相似</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Lyman_continuum&diff=4261Lyman continuum2026-01-19T08:18:53Z<p>Shen：</p>
<hr />
<div>*又写成LyC，比912A(13.6ev)波长更短的光子<br />
==escape fraction==<br />
*参考[http://arxiv.org/abs/1606.03452] [http://arxiv.org/abs/1606.05352]<br />
*本地星系的escapefraction在1%到10%<br />
*[[高红移星系]]中的escape fraction被认为/要求更高,这是宇宙的再电离要的。<br />
:高红移的UV光子的density是下降的<br />
*小质量的星系，escape fraction更高？[http://arxiv.org/abs/1606.05352]<br />
:burst模式的恒星形成，势井更浅，超新星会吹走部分其他，covering factor降低。</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83&diff=4260尘埃2026-01-14T14:50:01Z<p>Shen：/* 盘星系的尘埃分布 */</p>
<hr />
<div><br />
*发射线的消光可能和连续谱的消光不同<br />
*Halpha/Hbeta 线比<br />
:内禀数值：2.86（恒星形成），3.1（AGN） 参见Osterbrock & Ferland 2006<br />
*尘埃在8000A左右有一个Extended Red Emission(ERE)的连续谱发射<br />
*尘埃的红外发射: dustEM<br />
*尘埃与气体有关，气体的光深可以从low-ionization interstellar (IS) absorption lines(e.g., Si II, O I, Fe II)获得 (Shapley et al. 2003)<br />
:e.g. If the two Si II transitions at 1260 and 1527A are optically thin, then the ratio of their equivalent widths will be W1260/W1527 > 6. The observed ratio is W1260/W1527 ~ 1, implying that the lines are saturated and hence their depths are sensitive to the covering fraction of Si II-enriched material.<br />
<br />
:对于比912A更短的波长来说，气体的吸收消光是最主要的而不是dust，但是气体和尘埃是相关的，参见[http://arxiv.org/abs/1606.00434]<br />
*模型THEMIS The Heterogeneous dust Evolution Model for Interstellar Solids) [http://www.ias.u-psud.fr/themis/]<br />
<br />
==多波段==<br />
*DustPedia [https://arxiv.org/abs/1708.05335]<br />
:875个近距离星系 v<3000km/s<br />
:42 个波段 （UV - micro-wave）<br />
:孔径匹配 Comprehensive & Adaptable Aperture Photometry Routine (CAAPR)<br />
:这些星系的气体金属丰度（发射线），HI mass 等数据[https://arxiv.org/abs/1901.09040]<br />
<br />
*M31 1908.03458<br />
:*利用Herschel在300u的数据来估算M31中尘埃的辐射（PPMAP软件）<br />
:*同事利用近红外1.1mu的消光来估算尘埃的吸收<br />
:*这两个系数的比，发现M31中吸收/发射的数据比通常的模型小很多，说明很多尘埃只发射不吸收，（说明非常颗粒致密的尘埃源，行星？）<br />
<br />
==红外波段的吸收==<br />
* 1902.08326<br />
* 3.0um，有水吸收，3.4mu有芳香烃的吸收，都是要在Av很大的时候才有<br />
* 比如水在Av>3.2 的时候 才有Whittet 2001，芳香烃的吸收在Av小点地方就有<br />
* Si在9.7mu的吸收，这个Si吸收正比于Av<br />
* UV强的环境，水和芳香烃可能都更容易被破坏<br />
<br />
==尘埃成份==<br />
* [[PAH]] ，比例与金属丰度相关，金属丰度越高，PAH比例越高，银河系中大概5%，Remy-Ruyer 2015<br />
* 大颗粒粒子，是小颗粒粒子的两倍左右 Draine & Li 2001<br />
* 小颗粒粒子<br />
* C尘埃，石墨，无定型碳，AGB星的星风；硅酸盐尘埃，O尘埃，SN贡献（主要是II型超新星）Dwek 1996<br />
===[[消光曲线]]===<br />
*分子云中的turblence导致尘埃粒子按照颗粒大小分层分布，可以解释分子云中的消光曲线和其它地方不同[https://arxiv.org/abs/1706.05055]<br />
<br />
===尘埃散射===<br />
*arXiv:2201.01378 银河系中的尘埃散射可以造成银河系的背景光（Diffuse Galactic light），该文用天光光纤中光谱的涨落和同样位置的100mu的发射线强度进行相关，然后得到DGL，这个DGL基本可以用尘埃对星光的散射来解释<br />
<br />
==盘星系的尘埃分布==<br />
:可以延展到2R25，[http://arxiv.org/abs/1607.01020]:<br />
:密度轮廓比较follow恒星，而不是恒星形成（气体？）<br />
:有温度梯度，从中心25K到边缘15K<br />
:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象？<br />
:多波段结果进行对比[https://arxiv.org/abs/1706.05351]<br />
:高红移：气体分布比尘埃更延展 [https://arxiv.org/abs/1804.06852]<br />
:* 2601.02724 银河系的尘埃盘也可以分为薄盘和厚盘，薄盘和分子气体更相关，厚盘和原子气体相关<br />
<br />
==dust torus== <br />
* arXiv:2310.09093 the inner icy structure in local AGN<br />
<br />
==尘埃总量==<br />
*尘埃的总量可以通过基于能量平衡的SED拟合方法得到（如MAGPHYS），需要远红外数据如Herschel，如果考虑冷尘埃还需要亚毫米数据（如JCMT）<br />
*arXiv1910.06327 发现早型星系（SFR很低）中尘埃和恒星质量的比与星族年龄反相关，星族越老，尘埃越少，反映的尘埃的destruction time scale？（2Gyr）<br />
*[https://ui.adsabs.harvard.edu/abs/2013ApJ...766..121M/abstract]大概一半的，活动的椭圆星系中有大概10^5-6太阳质量的尘埃，这些尘埃是怎么来的？一般认为尘埃在早型星系中的存活时标较短（最多几万年）内部产生的，那不可能生成这么多次尘埃；如果外面吸积并合来的，要求较高的并合率，另外，为什么只在中心区域？<br />
* cosmic dust abundance,在z<1之后有所下降，认为椭圆星系的形成是主要原因 [https://arxiv.org/pdf/2302.03058.pdf]<br />
* 通过各种元素的丰度，加上depletion比例，及气体密度可以计算尘埃面密度（arXiv:2305.07743）<br />
===尘埃的来源===<br />
*AGB星（1.5-8个太阳质量）：貌似不可能是最主要机制，（AGB星占总恒星质量的大概10%，尘埃的产额最高0.01）Michalowsski et al. 2010<br />
*超新星 （同时可打散尘埃）<br />
*自己增长<br />
* [https://arxiv.org/pdf/2410.23959] 高红移的一些星系dust/star比例特别低，似乎没有进入自己增长的阶段（ISM dust）<br />
<br />
===气尘比 ===<br />
*一般说的气尘比是总气体，就是总的冷（温）气体<br />
:Planck 的结果说在Tau(353G)比较高(表征尘埃)的地方，气尘比略有下降<br />
*dust-to-gas (DGR) found in our Galaxy (NH/AV = 1.79 − 2.69 × 10^21 cm−2mag^-1)<br />
:MW中HI的体密度平均大概是1个H原子每cm^-3，对应的消光是E(B-V)/l= 0.61 mag/kpc [https://arxiv.org/abs/1906.10629]<br />
:在E(B-V)<0.04的时候，气体中的温气体开始贡献吸收；在E(B-V)>0.07的时候，H2开始出现，在中间的很窄范围内可能是HI主导<br />
*银河系盘外围区域的气尘比可能会偏大 [https://arxiv.org/abs/1708.05359]<br />
: We find a weak trend of decreasing infrared to ~20 cm flux density ratios with increasing Rgal, in agreement with previous extragalactic results, possibly indicating a decreased dust abundance in the outer Galaxy.<br />
*DGR与金属丰度有关，而且是线性相关，这可能说明DTM是常数<br />
*Remy-Ruyer et al. 2014, Sandstrom et al. 2013<br />
* ALMA探测到尘埃的热辐射的RJ波段（光学薄）可以装换为其它 ·902.08216<br />
<br />
<br />
===尘埃金属比===<br />
*dust-to-metals（DTM） ratio: 相比于DGR，DTM更可能是常数(MW)<br />
*M101中的DTM有变化 与f(H2)相：arXiv1808.07164<br />
:M(dust)/M(H)~0.0091Z/Zsun (Draine 2011, 2014)<br />
<br />
==尘埃的质量吸收系数==<br />
*这个系数与金属丰度相关（比较直观）<br />
*就是单位质量的尘埃能贡献多少红外辐射，和上面讨论的M31的近红外/远红外光深比类似<br />
*尘埃的质量怎么算？从气象金属丰度加上沉积模型算（1908.04318）<br />
*对M74和M83的估算，发现这个系数与local ISM的密度反相关（简单模型应该正相关，更高密度ISM的地方，尘埃粒子更容易生长，所以有更强的发射系数）（1908.04318）<br />
<br />
==模型==<br />
<br />
===化学演化模型===<br />
De Vis, P. MNRAS 2017<br />
<br />
===dust formation and destruction ===<br />
*formation: type II SNe,AGB, accretion of metals onto existing grains<br />
*destruction: SNe shocks, thermal evaporation, cosmic rays, incorporated into newly formed stars<br />
<br />
* dust depletion [Zn/Fe] 和 [X/Zn]之间很好的相关性 （1805.05365），前者表征尘埃，后者是不同元素结晶能力的不同，尘埃是慢慢生长出来的<br />
*尘埃的演化模型:2402.18515</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Bar&diff=4259Bar2025-12-29T10:34:21Z<p>Shen：</p>
<hr />
<div>*描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498]<br />
<br />
==strength==<br />
The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).<br />
* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010)<br />
* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al. (2002); Marinova & Jogee (2007); Aguerri et al. (2009)<br />
* Fourier decomposition of the galaxy light Ohta et al. (1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).<br />
<br />
==pattern speed==<br />
defined as the rotational frequency of the bar. <br />
* Bar cannot extend beyond the corotation resonance (CR) radius of the galaxy.<br />
* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed. <br />
* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.<br />
* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054<br />
<br />
==形成机制==<br />
* Can A Kinematically Hot and Thick Disk Form A Bar? : Role of Highly Spinning Dark Matter Halos arXiv:2512.21632 <br />
:*高红移星系，动力学上更热，看到了棒结构，可能与旋转的晕有关。</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=N/O&diff=4258N/O2025-12-04T10:41:29Z<p>Shen：</p>
<hr />
<div>*https://arxiv.org/abs/1911.00581<br />
*N/O ratio of 0.46 in GS 3073 at redshift z= 5.55：w can be produced by 1000 - 10,000 M⊙ primordial (Pop III) stars. [https://arxiv.org/abs/2502.04435]<br />
* All nitrogen-enhanced galaxies have moderate to high gas pressure () and high ionization parameter (), indicating a dense and compact environment. We suggest that super star clusters containing Wolf-Rayet stars and massive stars are the most likely contributors to the elevated nitrogen abundance in these galaxies. arXiv:2512.04043</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=PAH&diff=4257PAH2025-12-04T10:39:16Z<p>Shen：</p>
<hr />
<div>*PAH 的辐射<br />
:3.3um C-H键震动，脂肪族的C-H键震动在3.4um<br />
:6.2,7.6um是C-C拉伸震动<br />
:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲<br />
:17um,C-C-C弯曲，18mu有硅的发射特征<br />
* tight correlation of PAH and CO emission from z ∼ 0 to 4 [https://arxiv.org/pdf/2409.05710]<br />
:* PAH和CO与IR光度的关系都是sub-linear的，MIR的光度中有AGN的贡献<br />
<br />
*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]<br />
<br />
* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.2697（很好的一篇review）<br />
<br />
*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102 <br />
<br />
* PAHs can form and survive in extremely metal-poor environments https://arxiv.org/abs/2512.04060 JWST Captures Growth of Aromatic Hydrocarbon Dust Particles in the Extremely Metal-poor Galaxy Sextans A<br />
<br />
*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]<br />
*[[PAHFIT]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=NSC&diff=4256NSC2025-12-04T10:37:08Z<p>Shen：</p>
<hr />
<div>nuclear star cluster<br />
arXiv:2405.14948<br />
* NSC的质量和暗晕质量相关性似乎更好，这一点和星系中的球状星团类似。<br />
* 非常年老，贫金属 https://arxiv.org/abs/2512.03999 The Nuclear Star Cluster of M 74: a fossil record of the very early stages of a star-forming galaxy</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=PAH&diff=4255PAH2025-11-06T03:03:20Z<p>Shen：</p>
<hr />
<div>*PAH 的辐射<br />
:3.3um C-H键震动，脂肪族的C-H键震动在3.4um<br />
:6.2,7.6um是C-C拉伸震动<br />
:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲<br />
:17um,C-C-C弯曲，18mu有硅的发射特征<br />
* tight correlation of PAH and CO emission from z ∼ 0 to 4 [https://arxiv.org/pdf/2409.05710]<br />
:* PAH和CO与IR光度的关系都是sub-linear的，MIR的光度中有AGN的贡献<br />
<br />
*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]<br />
<br />
* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.2697（很好的一篇review）<br />
<br />
*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102 <br />
<br />
*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]<br />
*[[PAHFIT]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=PAH&diff=4254PAH2025-11-06T03:00:34Z<p>Shen：</p>
<hr />
<div>*PAH 的辐射<br />
:3.3um C-H键震动，脂肪族的C-H键震动在3.4um<br />
:6.2,7.6um是C-C拉伸震动<br />
:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲<br />
:17um,C-C-C弯曲，18mu有硅的发射特征<br />
* tight correlation of PAH and CO emission from z ∼ 0 to 4 [https://arxiv.org/pdf/2409.05710]<br />
:* PAH和CO与IR光度的关系都是sub-linear的，MIR的光度中有AGN的贡献<br />
<br />
*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]<br />
<br />
* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.2697<br />
<br />
*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102 <br />
<br />
*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]<br />
*[[PAHFIT]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4253尘埃粒子的分布2025-11-05T11:45:03Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math> N(a) \propto a^{-3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4252尘埃粒子的分布2025-11-05T11:44:51Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math> N(a) ~ a^{-3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4251尘埃粒子的分布2025-11-05T11:44:34Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math> N(a) ~ a^{−3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4250尘埃粒子的分布2025-11-05T11:44:24Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math> N(a) $\sim$ a^{−3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4249尘埃粒子的分布2025-11-05T11:43:50Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math>E=mc^2</math><br />
<br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4248尘埃粒子的分布2025-11-05T11:43:33Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<math>E=mc^2</math><br />
<math> N(a)\propto a^{−3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4247尘埃粒子的分布2025-11-05T11:32:29Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <br />
<br />
<math> N(a)\propto a^{−3.5} </math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E5%B0%98%E5%9F%83%E7%B2%92%E5%AD%90%E7%9A%84%E5%88%86%E5%B8%83&diff=4246尘埃粒子的分布2025-11-05T11:29:27Z<p>Shen：</p>
<hr />
<div>Ref. http://arxiv.org/abs/astro-ph/0603833<br />
<br />
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <math>N(a)\propto a^{−3.5}</math><br />
:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.<br />
:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;<br />
<br />
*BF model: Bianchi & Ferrara (2005) <br />
:assuming an initial flat size abundance <br />
:the post-processed distribution remains nearly flat <br />
:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering<br />
<br />
*尘埃到行星，粒子分布的gap？arXiv:2511.01957</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Quiescent_galaxies&diff=4245Quiescent galaxies2025-11-05T11:28:18Z<p>Shen：创建页面，内容为“* arXiv:2511.02045: galaxies with weak emission lines, referred to as retired (R), and those without emission lines, dubbed passive (P),这两类星系之间的差异来自于warm gas （环境因素）”</p>
<hr />
<div>* arXiv:2511.02045: galaxies with weak emission lines, referred to as retired (R), and those without emission lines, dubbed passive (P),这两类星系之间的差异来自于warm gas （环境因素）</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E6%96%87%E7%8C%AE%EF%BC%9A%E6%98%9F%E7%B3%BB&diff=4244文献：星系2025-11-05T11:26:11Z<p>Shen：/* 发射线 */</p>
<hr />
<div>==高红移星系== <br />
<br />
* high redshift galaxies (z>5) are not as blue as before reported(arXiv:1102.4881, arXiv:1102.5005)<br />
*亚毫米星系The intense star formation rates are fueled in part by a reservoir gas supply enabled by stellar feedback at earlier times, not through major mergers. Nature 文章 [http://arxiv.org/abs/1509.06377]<br />
*CR7 (cosmic redshift 7): Ly emitter，z=6.604 [http://arxiv.org/pdf/1504.01734]<br />
:population III 星系？ [http://arxiv.org/abs/1602.04843]<br />
*z>1的恒星形成模式主要是[[disk instability]]? [http://arxiv.org/abs/1606.06739]<br />
*z~9： Brightest of Reionizing Galaxies Survey (BoRG[z9]) pure-parallel HST [arXiv:1809.07604]<br />
* Till Sep. 2022, the only spectroscopically confirmed galaxy at 𝑧>10 is GN-z11 (Oesch et al. 2016).<br />
<br />
===z~1===<br />
*the basic trends observed in the local universe were already established at z∼1.3, i.e. more massive spheroids are more metal rich, have lower stellar mass density and tend to be older than lower-mass galaxies. arXiv:1901.01595<br />
<br />
==环境==<br />
*arXiv:1103.0259 <br />
<br />
ETGs belonging to the cluster environment host on average older stars with respect to group and fieldpopulations. This difference is less significant than the age difference in galaxies of different masses.<br />
*arXiv:1103.0265: <br />
Thus we conclude that while galaxy mass regulates the timing of galaxy formation, the environment regulates the timescale of their star formation histories.<br />
*[http://arxiv.org/abs/1607.03318]<br />
:小质量的satellite受环境作用影响较大。大质量的satelite和central一样，主要受星系中心速度弥散度影响。<br />
<br />
*nature vs nurture [https://arxiv.org/abs/1805.12175]<br />
:红移到0.9的星系团，星系的mass-SFR relation已经存在了<br />
<br />
==发射线==<br />
*[OIII]/Hbeta：很好的trace sSFR [ arXiv:1606.01259]<br />
* low ionisation emission line regions '''LIER''' [http://arxiv.org/abs/1609.01737]<br />
:基于[[MaNGA]]的结果.这些发射线是热星引起，与恒星形成的quench有关，不是[[AGN]]<br />
:老年星系：一些有发射线，一些没有 [[quiescent galaxies]] devoid of line emission reside in denser environments and have significantly higher satellite fraction than eLIERs. Environmental effects thus represent the likely cause for the existence of line-less galaxies on the red sequence.<br />
*从发射线推导金属丰度等信息：[https://arxiv.org/abs/1803.10236 GAME] PYQZ [[HII-CHI-MISTRY]]<br />
<br />
==恒星形成历史==<br />
*resolved [[SFH]] from [[CMD]] arXiv 1509.96647 [http://arxiv.org/abs/1509.06647]<br />
:IAC-STAR SYNTHETIC COLOR-MAGNITUDE DIAGRAM COMPUTATION ALGORITHM [http://iac-star.iac.es/cmd/index.htm]<br />
<br />
*恒星形成停止的机制<br />
:Nature文章，从金属丰度的角度来看有意思。Strangulation as the primary mechanism for shutting down star formation in galaxies [http://arxiv.org/abs/1505.03143]<br />
<br />
*arXiv 1109.2905<br />
:[[Halpha]]作为SFR的indicator 是age小于5Myr的M大于15Msun的恒星。UV luminosity是M大于3Msun的恒星贡献，时标为 <300Myr。<br />
:Halpha和 L UV得到的SFR有系统差异，主要表现在低质量星系当中，弥散大，Halpha得到的SFR系统偏低。<br />
:Solution I： Integrated galactic IMF的不同。（Lee et al. 2009)，cluster IMF 和culster mass function 积分才能得到星系的IMF，小质量星系中大质量cluster 少，所以大质量恒星少，从而造成Halpha 得到的SFR偏低。<br />
:本文的solution：由于小质量星系的SFH不是constant，二是burst模式造成的，burst强度大概30，时标大概在250Myr.<br />
:*comment：看上去有点玄，文章最后给出的Hubble的CMD得到的SFH增强了一点说服力。<br />
<br />
*arXiv 1809.06380<br />
:和上面的工作很相像，进一步引入了M*-LHa上的偏离这个量，并按照不同恒星质量分bin，分别研究Delta LHa和LHa/LUV的关系<br />
<br />
* arXiv:1109.2597<br />
:[[Balmer decrement]]可以用来研究星系的消光性质，但是需要emission line 中扣除 A型恒星的absorbation line。<br />
:对低分辨率光谱，这个absorbation line的扣除很难。<br />
:本文提出你用等值宽度的比来替代传统的流量比的方法。<br />
:absorption line的等值宽度接近一个常数。<br />
:附加内容：从MPA/JHU DR7 SDSS galaxy sample 的Balmer decrement得到 的消光曲线有系统偏差，认为是H\beta的测量存在系统差。<br />
<br />
===质量增长历史===<br />
*1710.08421<br />
:利用数密度，从质量函数里面计算给定质量的星系其平均的质量增长历史，从而计算assembly time（质量增长一半）,同时计算这些星系的星族的平均年龄。<br />
:比较这两个时标，发现大质量星系的星族的平均年龄要大于assembly time，这说明大质量星系中的很多恒星是外来（吸积）的。<br />
<br />
*1903.11089 <br />
:从光谱里得吸积历史（基本上是神话）<br />
:用ppxf的regu来得恒星形成历史的地方可以参考一下<br />
<br />
<br />
===化学增丰历史===<br />
<br />
==main sequence==<br />
<br />
*SFR-M* relation在低质量段： 线性的？[https://arxiv.org/abs/1808.04900](红移演化？）<br />
*SFR-M*的关系：与星系分类有关，pure的star forming galaxy（BPT diagram）的线性较好，composite， LINER，AGN等会turn over[https://arxiv.org/abs/1810.10021]<br />
:pure 的SF星系，SSFR最高的部分，B/T反而相对比较大，为什么？？？<br />
*利用一个随机过程来描述 main sequence的涨落，想法很好，introduction写得很好 arXiv:1901.07556<br />
*arXiv:2310.03081 高红移星系的SFMS （z~3-12）<br />
<br />
<br />
===resolved main sequence===<br />
*arXiv 1803.00319: 星系按照D4000的轮廓分为两类，inside out的 星系在内部区域其恒星形成效率似乎受到抑制<br />
*arXiv 2201.03592: resolved SFMS 可能不是物理本质，而是由resolved KS和resolved Molecular gas-stellar surface density relation引起的[[ALMaQUEST]]<br />
<br />
==气体==<br />
===冷气体===<br />
*星系的气（HI+H2）尘比对环境的依赖性很弱（从isolated 到 virgo cluster）,团星系同样的气体，尘埃略多[http://arxiv.org/abs/1604.01505]<br />
===温气体===<br />
* 1606.04536 直接探测到温气体的晕，OVI 1032,1038 doublet [http://arxiv.org/abs/1606.04536]<br />
===热气体===<br />
<br />
*椭圆星系的热气体 Borosn et al. 2011 (ApJ, 729, 12)<br />
:Chandra观测的30个ETG （non-CD)星系的热气体成份。发现很多gas-poor的低X射线光度星系(10^38 erg s^-1)，在给定光学光度的地方Lx可以有3个量级的差异。温度比维里温度预言的要高（ arXiv: 1106.2898)。<br />
:但是，整体来说，热气体温度正比于光度。 （kT>0.4KeV的是高光度的，而kT<0. 3KeV的低光度）。<br />
:这个结果和外流模型的预言不同，外流模型中，低光度因为气体外流后，热气体密度降低引起的，但外流的气体应该有较高的温度，因此光度和温度之间是反相关。<br />
<br />
<br />
<br />
==其它==<br />
<br />
*arXiv:1110.6320<br />
说early type galaxy fraction与halo mass基本无关，但是是galaxy stellar mass的<br />
function。这基本上说明，cluster member 的LF和filed 差不多。<br />
<br />
*arXiv:1201.3374<br />
The observations show that dust gradients are indeed typically steeper than the corresponding metallicity gradients.<br />
<br />
*arXiv:1201.2727 星系的指向<br />
HST的image测量z>0.<br />
5的星系团中星系的alignment的指向，发现500Kpc以内的星系基本上没有特殊的指向。<br />
红星系可能有，但统计上不显著。<br />
这和低红移z ～ 0.1 的结果差异比较大。<br />
解释：显著演化效应还是SDSS的image分析有系统bias？<br />
<br />
*arXiv:1112.3704<br />
Galaxies(at z~1.4) with higher SFR and larger half light radii show lower metallicities at a given stellar mass.<br />
<br />
*dense low mass early type galaxy arXiv 1111.2905<br />
考察这一类星系在FP上，发现基本完全遵循维里定理，这说明暗物质影响不大，物质分布完全遵循光度分布。<br />
因此，从光度分布可以直接导出动力学质量（假设球对称的Jeans方程）。<br />
对比星族合成得到的恒星质量和动力学质量可以从而用来约束IMF。<br />
方法看上去不错，但是最后得到IFM和颜色有关，这个结论看上去有点可疑。<br />
size和颜色基本不相关，由维里定律可知，这个动力学质量也就基本和颜色无关。<br />
恒星质量显然是颜色相关，导出合格IMF与颜色相关也就不足为奇。<br />
<br />
*早型星系中的发射线星系。 1103.3652<br />
大部分O[III]的EW基本是一个常数0.75AA，说明发射线很可能是恒星起源的。(按照BPT图分为 LINEAR）<br />
恒星起源：<br />
#evolved stars post AGN, white dwarf<br />
#Shocks ,supernova<br />
一小部分EW大的则可能是AGN起源。<br />
<br />
*CD星系的Abell 2199 的速度弥散度的profile [http://arxiv.org/abs/1411.2598 arXiv1411.2598]<br />
:从心的200km/s（星系的引力势井） 增加到外围的850km/s （由星系团决定）<br />
<br />
＊光致电离<br />
:考察了一些本地的高电离度的星系，发现要合理的解释电离线比要求models with an escape fraction of ionizing photons lower than 10%［http://arxiv.org/abs/1503.00320］<br />
===intra-group medium===<br />
*[http://arxiv.org/abs/1607.03386]<br />
:Probing the intra-group medium of a z = 0.28 galaxy group using [[MUSE]] and background QSO, favour the latter, in which the cool gas belongs to the intra-group medium and is likely pressure confined within a warmer gas halo.<br />
<br />
<br />
==模型==<br />
*IKEA model [https://arxiv.org/abs/1906.10135]<br />
==专题==<br />
[[文献：IMF]]<br />
<br />
[[文献：Size evolution]]<br />
<br />
[[文献：scaling relation]]<br />
<br />
[[文献：cosmic star formation history]]<br />
<br />
[[文献：IFU]]<br />
<br />
[[文献：outflow]]<br />
<br />
[[文献：passive disk/red spiral]]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=AGN%E7%9A%84%E5%85%89%E5%8F%98&diff=4243AGN的光变2025-11-05T10:42:33Z<p>Shen：</p>
<hr />
<div>*[http://arxiv.org/abs/1607.04297]<br />
*An Extremely Luminous Flare https://arxiv.org/abs/2511.02178</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=Bar&diff=4242Bar2025-11-05T10:39:38Z<p>Shen：</p>
<hr />
<div>*描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498]<br />
<br />
==strength==<br />
The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).<br />
* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010)<br />
* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al. (2002); Marinova & Jogee (2007); Aguerri et al. (2009)<br />
* Fourier decomposition of the galaxy light Ohta et al. (1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).<br />
<br />
==pattern speed==<br />
defined as the rotational frequency of the bar. <br />
* Bar cannot extend beyond the corotation resonance (CR) radius of the galaxy.<br />
* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed. <br />
* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.<br />
* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E4%B8%AA%E4%BA%BA%E7%AE%80%E5%8E%86&diff=4241个人简历2025-10-22T02:03:40Z<p>Shen：</p>
<hr />
<div>'''沈世银'''<br />
:博士，研究员，博士生导师<br />
:上海天文台天体物理研究室《星团和银河系结构》课题组组长。<br />
:地址：上海市南丹路80号，200030<br />
:电话：021-34775318 ； 电子邮件：ssy@shao.ac.cn<br />
<br />
'''职业经历'''<br />
:* 2011/9 – 至今，上海天文台，研究员。<br />
:* 2004/9 – 20011/8, 上海天文台，助理研究员，副研究员；<br />
:* 2003/9 – 2004/8, 德国马普天体物理研究所，博士后；<br />
<br />
'''教育经历'''<br />
:* 2001 年 3 月 - 2003 年 8 月，德国马普天体物理研究所，交换项目博士研究生。<br />
:* 1998 年 9 月 - 2001 年 2 月，上海天文台，天体物理专业，硕士研究生；<br />
:* 1994 年 9 月 - 1998 年 7 月，重庆大学，应用化学专业，学士学位；<br />
<br />
'''学术兼职'''<br />
:* 郭守敬望远镜（LAMOST）科学委员会委员<br />
:*《天文学进展》副主编<br />
:*《天文学报》编委<br />
<br />
'''学术荣誉'''<br />
:* 爱思唯尔“中国高被引学者”<br />
:* 上海市优秀学术带头人（2022）<br />
:* 银河系尘埃三维分布的研究[https://ui.adsabs.harvard.edu/abs/2018ApJ...858...75L/abstract]获评中国十大天文进展之一（2018）<br />
:* 中科院青年创新促进会会员（2012）<br />
:* 中科院卢嘉锡青年人才奖(2010)<br />
:* 上海市科技启明星（2008）<br />
:* 上海市自然科学二等奖（2007,2024）</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=%E4%B8%AA%E4%BA%BA%E7%AE%80%E5%8E%86&diff=4240个人简历2025-10-22T02:03:07Z<p>Shen：</p>
<hr />
<div>'''沈世银'''<br />
:博士，研究员，博士生导师<br />
:上海天文台天体物理研究室《星团和银河系结构》课题组组长。<br />
:地址：上海市南丹路80号，200030<br />
:电话：021-34775318 ； 电子邮件：ssy@shao.ac.cn<br />
<br />
'''职业经历'''<br />
:* 2011/9 – 至今，上海天文台，研究员。<br />
:* 2004/9 – 20011/8, 上海天文台，助理研究员，副研究员；<br />
:* 2003/9 – 2004/8, 德国马普天体物理研究所，博士后；<br />
<br />
'''教育经历'''<br />
:* 2001 年 3 月 - 2003 年 8 月，德国马普天体物理研究所，交换项目博士研究生。<br />
:* 1998 年 9 月 - 2001 年 2 月，上海天文台，天体物理专业，硕士研究生；<br />
:* 1994 年 9 月 - 1998 年 7 月，重庆大学，应用化学专业，学士学位；<br />
<br />
'''学术兼职'''<br />
:* 郭守敬望远镜（LAMOST）科学委员会委员<br />
:* 《天文学进展》副主编、《天文学报》编委<br />
<br />
'''学术荣誉'''<br />
:* 爱思唯尔“中国高被引学者”<br />
:* 上海市优秀学术带头人（2022）<br />
:* 银河系尘埃三维分布的研究[https://ui.adsabs.harvard.edu/abs/2018ApJ...858...75L/abstract]获评中国十大天文进展之一（2018）<br />
:* 中科院青年创新促进会会员（2012）<br />
:* 中科院卢嘉锡青年人才奖(2010)<br />
:* 上海市科技启明星（2008）<br />
:* 上海市自然科学二等奖（2007,2024）<br />
<br />
'''论文发布'''<br />
*[https://ui.adsabs.harvard.edu/search/q=orcid%3A0000-0002-3073-5871&sort=date%20desc%2C%20bibcode%20desc&p_=0 论文目录]</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=CV:_English&diff=4239CV: English2025-10-22T02:02:13Z<p>Shen：</p>
<hr />
<div>'''Prof. Dr. Shiyin Shen'''<br />
:Nandan Road, 80， Shanghai Astronomical Observatory，Chinese Academy of Sciences, Shanghai, 200030<br />
:Tel: 0086-21-34775318<br />
<br />
'''Education'''<br />
:*B.S., Applied Chemistry，1998, ChongQing University<br />
:*Ph.D., Astrophysics, 2003, Graduated university of CAS<br />
:* Mar. 2001 - Aug. 2003, Max-Planck Institute of Astrophysics, Exchange student<br />
<br />
'''Professional Experience'''<br />
:*Aug. 2003 – Aug. 2004, Max-Planck Institute of Astrophysics, Post doctor<br />
:*Sep. 2004 – so far, Shanghai Astronomical Observatory, assistant professor, associate professor, professor<br />
<br />
'''Awards'''<br />
:* Shanghai Academic Research Leader (2022)<br />
:* Highly Cited Chinese Researchers of Elsevier <br />
:*The study on the dust geometry of Milky-Way[https://ui.adsabs.harvard.edu/abs/2018ApJ...858...75L/abstract] is awarded as one of the top 10 advances of the Chinese astronomy （2018）<br />
:*LUJIAXI young Scholarship (2010)<br />
:*Shanghai Rising-Star Program (2008)<br />
:*Shanghai natural sciences second prize (2007，2024)<br />
<br />
'''Services'''<br />
:*LAMOST Scientific Committee Member<br />
:*Deputy Editor-in-Chief of Progress in Astronomy<br />
:*Science Editor of Acta Astronomica Sinca</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=CV:_English&diff=4238CV: English2025-10-22T02:01:52Z<p>Shen：</p>
<hr />
<div>'''Prof. Dr. Shiyin Shen'''<br />
[[文件:Me.jpg|right|150px|shen]]<br />
:Nandan Road, 80， Shanghai Astronomical Observatory，Chinese Academy of Sciences, Shanghai, 200030<br />
:Tel: 0086-21-34775318<br />
:E-mail：ssy@shao.ac.cn<br />
<br />
'''Education'''<br />
:*B.S., Applied Chemistry，1998, ChongQing University<br />
:*Ph.D., Astrophysics, 2003, Graduated university of CAS<br />
:* Mar. 2001 - Aug. 2003, Max-Planck Institute of Astrophysics, Exchange student<br />
<br />
'''Professional Experience'''<br />
:*Aug. 2003 – Aug. 2004, Max-Planck Institute of Astrophysics, Post doctor<br />
:*Sep. 2004 – so far, Shanghai Astronomical Observatory, assistant professor, associate professor, professor<br />
<br />
'''Awards'''<br />
:* Shanghai Academic Research Leader (2022)<br />
:* Highly Cited Chinese Researchers of Elsevier <br />
:*The study on the dust geometry of Milky-Way[https://ui.adsabs.harvard.edu/abs/2018ApJ...858...75L/abstract] is awarded as one of the top 10 advances of the Chinese astronomy （2018）<br />
:*LUJIAXI young Scholarship (2010)<br />
:*Shanghai Rising-Star Program (2008)<br />
:*Shanghai natural sciences second prize (2007，2024)<br />
<br />
'''Services'''<br />
:*LAMOST Scientific Committee Member<br />
:*Deputy Editor-in-Chief of Progress in Astronomy<br />
:*Science Editor of Acta Astronomica Sinca</div>Shenhttp://202.127.29.3/~shen/wiki/index.php?title=About_Me&diff=4237About Me2025-10-22T02:01:17Z<p>Shen：</p>
<hr />
<div>'''Prof. Dr. Shiyin Shen ''' (ssy@shao.ac.cn)<br />
* orcid: 0000-0002-3073-5871<br />
* leader of the research group '''[http://cluster.shao.ac.cn Star cluster and Galaxies]''';<br />
<br />
== Research Interests ==<br />
* AI-related applications on galaxy structure and morphology [https://ui.adsabs.harvard.edu/#abs/2023MNRAS.526.6391X/abstract][https://arxiv.org/abs/2412.15533][https://arxiv.org/abs/2410.21962][https://arxiv.org/abs/2404.07780]<br />
* dust geometry of MW and local disk galaxies [http://adsabs.harvard.edu/abs/2017AJ....153...88L][http://adsabs.harvard.edu/abs/2018ApJ...858...75L][https://ui.adsabs.harvard.edu/#abs/2022ApJ...938..139L/abstract][https://ui.adsabs.harvard.edu/#abs/2023ApJ...946L...7L/abstract]<br />
* galaxy interaction, galaxy pair, compact groups of galaxies [https://ui.adsabs.harvard.edu/abs/2016RAA....16...43S/abstract] [https://ui.adsabs.harvard.edu/#abs/2019ApJ...880..114F/abstract] [https://ui.adsabs.harvard.edu/abs/2020ApJS..246...12Z/abstract][https://ui.adsabs.harvard.edu/#abs/2022ApJ...926..119Z/abstract][https://ui.adsabs.harvard.edu/#abs/2021ApJ...911..105Z/abstract][https://ui.adsabs.harvard.edu/#abs/2020ApJS..246...12Z/abstract]<br />
* IFS study of nearby galaxies [https://ui.adsabs.harvard.edu/abs/2018A%26A...613A..13Y/abstract] [https://ui.adsabs.harvard.edu/#abs/2020ApJ...892L..20F/abstract] [https://ui.adsabs.harvard.edu/#abs/2024ApJ...976...15Q/abstract][https://ui.adsabs.harvard.edu/#abs/2024ApJ...977..175L/abstract] [https://ui.adsabs.harvard.edu/#abs/2022ApJS..262....6F/abstract]<br />
<br />
==Research highlights==<br />
* AI applications on galaxy images: how many latent features can effectively represent a main sample galaxy image(r<17.77) in DESI? The answer is 40. [https://ui.adsabs.harvard.edu/#abs/2023MNRAS.526.6391X/abstract]<br />
* The Chocolate Chip Cookie Model: Dust Geometry of Milky Way-like Disk Galaxies [https://ui.adsabs.harvard.edu/#abs/2022ApJ...938..139L/abstract]<br />
* How to quntify the interaction level of paired galaxies? Kinemetry~ [https://ui.adsabs.harvard.edu/#abs/2020ApJ...892L..20F/abstract]<br />
* How to model the three-dimensional dust distribution of MW? What is the vertical distance of the Sun to the Galactic plane? [http://adsabs.harvard.edu/abs/2018ApJ...858...75L]<br />
* LAMOST Complementary galaxy sample: these galaxies in SDSS main galaxy sample without spectroscopy [https://ui.adsabs.harvard.edu/abs/2016RAA....16...43S/abstract]<br />
* Whether the universe is transparent? [https://ui.adsabs.harvard.edu/abs/2015ApJ...802L..16X/abstract]<br />
* Are the brightest group/cluster galaxies special? Is it only because of their definition? [http://adsabs.harvard.edu/abs/2014ApJ...782...23S]<br />
* The size distribution (size-mass relation) of local galaxies [https://ui.adsabs.harvard.edu/abs/2003MNRAS.343..978S/abstract]<br />
<br />
==Curriculum Vitae 个人简历 ==<br />
*[[CV: English]]<br />
*[[个人简历]]<br />
<br />
==Links==<br />
*[http://cluster.shao.ac.cn/~shen/PhD/THESIS.pdf 博士论文：星系大小分布的统计研究]<br />
*[https://ui.adsabs.harvard.edu/search/q=orcid%3A0000-0002-3073-5871&sort=date+desc My Publications]</div>Shen