text:
Q: Spring Boot - How to disable @Cacheable during development? I'm looking for 2 things:

*

*How to disable all caching during development with Spring boot "dev" profile. There doesn't seam to be a general setting to turn it all off in application.properties. What's the easiest way?

*How to disable caching for a specific method? I tried to use SpEl like this:
@Cacheable(value = "complex-calc", condition="#${spring.profiles.active} != 'dev'}")
public String someBigCalculation(String input){
   ...
}

But I can get it to work. There are a couple of questions on SO related to this, but they refer to XML config or other things, but I'm using Spring Boot 1.3.3 and this uses auto-configuration.
I don't want to over-complicate things.

A: The type of cache is by default automatically detected and configured. However you can specify which cache type to use by adding spring.cache.type to your configuration. To disable it set the value to NONE.
As you want to do it for a specific profile add it to that profiles application.properties in this case modify the application-dev.properties and add
spring.cache.type=NONE

This will disable caching.

A: The  David Newcomb comment tells the truth :

spring.cache.type=NONE doesn't switch caching off, it prevents things
  from being cached. i.e. it still adds 27 layers of AOP/interceptor
  stack to your program, it's just that it doesn't do the caching. It
  depends what he means by "turn it all off".

Using this option may fast up the application startup but could also have some overheads.
1)To disable completely the Spring Cache feature
Move the @EnableCaching class in a dedicated configuration class that we will wrap with a @Profile to enable it :
@Profile("!dev")
@EnableCaching
@Configuration
public class CachingConfiguration {}

Of course if you already have a Configuration class that is enabled for all but the dev environment, just reuse it :
@Profile("!dev")
//... any other annotation
@EnableCaching
@Configuration
public class NoDevConfiguration {}

2) Use a fake (noop) Cache manager
In some cases, activating @EnableCaching by profile is not enough because some of your classes or some Spring dependencies of your app expect to retrieve from the Spring container a bean implementing the org.springframework.cache.CacheManager interface.
In this case, the right way is using a fake implementation that will allow Spring to resolve all dependencies while the implementation of the CacheManager is overhead free.
We could achieve it by playing with @Bean and @Profile :
import org.springframework.cache.support.NoOpCacheManager;

@Configuration
public class CacheManagerConfiguration {

    @Bean
    @Profile("!dev")
    public CacheManager getRealCacheManager() {
        return new CaffeineCacheManager();
        // or any other implementation
        // return new EhCacheCacheManager();
    }

    @Bean
    @Profile("dev")
    public CacheManager getNoOpCacheManager() {
        return new NoOpCacheManager();
    }
}

Or if it is more suitable, you can add the spring.cache.type=NONE property that produces the same result as written in the   M. Deinum answer.

A: For your second question do something like this:
Write a method that determines whether or not a particular profile is active (environment is your injected Environment)
boolean isProfileActive(String profile) {
   return Arrays.asList(environment.getActiveProfiles()).contains(profile);
}

then use that for your spel condition on the cacheable annotation

A: If you have just a default profile and don't want to go through creating a dev and prod profiles just for this, I think this could be a very quick solution for your project:
Set this in your application.properties:
appconfig.enablecache=true

Based on your requirements, you can change it to true/false.
Now, when defining your @Caching bean, do this:
@Bean
public CacheManager cacheManager(@Value("${appconfig.enablecache}") String enableCaching) {
    if (enableCaching.equals("true")) {
        return new EhCacheCacheManager();
        //Add your Caching Implementation here.
    }
    return new NoOpCacheManager();
}

When property is set to false, NoOpCacheManager() is returned, effectively switching off your caching.

A: In any class you want to globally enable or disable your caching, on a per method basis, you can do the following, which allows you to control at the class level how your methods are cached.
You can change it in application.properties with my.cache.enabled=true. This setup currently defaults to it being enabled.
Of course then you can change it in application-dev.properties as well, and set it to a different value. The advantage of this approach is it lets you make this more complex if you need to for some reason, on a per method basis as well.
public class MyClass {

  @Value("${my.cache.enabled:true}")
  public String isMyCacheEnabled;

  public boolean isMyCacheEnabled() {
    return (isMyCacheEnabled == null) || isMyCacheEnabled.equals("") || Boolean.valueOf(isMyCacheEnabled);
  }

  @Cacheable(
      cacheManager = "myCacheManager",
      cacheNames = "myCacheKey",
      condition = "#root.target.isMyCacheEnabled()",
      key = "#service + '-' + #key")
  public String getMyValue(String service, String key) {
    // do whatever you normally would to get your value
    return "some data" + service + key;
  }
}

redpajama_set_name: RedPajamaStackExchange


text:
Epigraphie, calligraphie, codicologie, littérature
Max van Berchem
Marguerite van Berchem
Thesaurus d'Epigraphie Islamique
Vous trouverez ici la liste complète des projets soutenus par la Fondation Max van Berchem, classés par domaines d'activité, avec indication des dates de ce soutien.
Dans chaque domaine d'activité, les projets publiés dans le Bulletin sont soulignés.
THE MARCEL COLLECTION IN THE NATIONAL LIBRARY OF RUSSIA | 2004
EPIGRAPHIE, CALLIGRAPHIE, CODICOLOGIE, LITTERATURE / EPIGRAPHY, CALLIGRAPHY, CODICOLOGY, LITERATURE
POLOSIN Valéry et VASILYEVA Olga
The National Library of Russia (former Imperial Public Library) in St.-Petersburg houses an extensive and valuable collection of Oriental manuscripts originating mostly from the Near East. One of the library's treasures is the collection of Koran fragments written in so-called "Kufi" script. This collection was assembled by the French orientalist J.-J. Marcel, and acquired by the library in 1864 from his heirs due to the efforts of the Russian orientalist Nicholas Khanykoff who then lived in Paris.
Jean Joseph Marcel (1776-1854) was among the participants of Napoleon's war expedition in Egypt. In 1798-1801 he was the head of Imprimerie Nationale in Alexandria and Cairo. During these years he became educated in the Arabic language and history to the extent, which later allowed him to compile the Arabic-French dictionary and write interesting articles on the history of Egypt. At the same time he was collecting antiquities. Unfortunately of his extensive collection, of which only manuscript part contained 3000 items, solely the 8-11th centuries "Kufi" Koran fragments have survived as an entity. He collected most of these fragments in the oldest mosque in Cairo, built by 'Amr b. al-'As in 643.
Qur'an fragment from the J.-J. Marcel collection. Sura 2:173 (10th century, 228 ? 325 mm
(National Library of Russia, Marcel 64, fol. 4 v.)
The Library acquired the collection together with the hand-list made by Victor Langlois. This hand-list consisted of three parts and contained descriptions of 119 items (the third part consisted of one 15th century Koran volume and personal papers of Marcel). Later some of the items were divided into separate fragments, and nowadays the total number of items in Marcel collection is 132, of them 129 - "Kufi" fragments (2000 folios).
Our project is a complex one and involves two main types of activities. First, activities aimed at the conservation of the manuscripts, including:
a. improvement of the conservation conditions (providing the manuscripts with the new covers made of acid-free paper, moving the manuscripts into a special safe storage);
b. conservation and restoration works on some of the items;
c. making digital copies of the first pages and illuminated pages of every item;
d. microfilming the entire collection.
Second, activities aimed at the creation of the electronic catalogue of the collection. The basis of the catalogue is the traditional description of the fragments made according to the system, proposed by F. Déroche in his catalogues: "Les manuscrits du Coran : Aux origines de la calligraphie coranique" [Bibliothèque - Nationale, Catalogue des manuscrits arabes, 2e partie, Manuscrits musulmans, I/1], Paris, 1983; "The Abbasid tradition, Qur'ans of the 8th to the 10th centuries" [The Nasser D. Khalili collection of Islamic art, I], London, 1992. However two more points were added to this system: incipits and explicits of the fragments and the bigger to smaller dimensions ratio of the manuscript (folio and text field).
This data will be registered in the information retrieval system "Depository" which has been created for the electronic catalogue of the Manuscript Department of the National Library of Russia. This system comprises the detailed structure of the fields and basic references, its main fields corresponding with the standard format accepted by the Library, which allows to convert the data into modern international standards. The system had been tested on the material of Slavonic manuscripts. To achieve the aims of our project certain adaptations were made in the database; attributive features of the hand-written Korans were determined; new blocks of fields were added according to the specific of the material; new terminology and graphic (for the description of the elements of illumination) references formed and tested. Four print-out formats of the description will be available in the electronic catalogue: 1) brief inventory record; 2) full analytic description; 3) full analytic description with commentaries; 4) check format showing the information as it is registered in the fields of the database.
The catalogue will be prefaced with the articles about the history of the Marcel collection, principles of the manuscripts description and the directions for the users of the catalogue.
The main aim of the project is preparation of the text and images for the publication of a catalogue in the form of a book and/or CD-ROM, which may be regarded as the first issue of the catalogue of the Arabic manuscripts in the National library of Russia collections.
Olga Vasilyeva
Valery Polosin
Ekaterina Krushelnitskaya
Site réalisé par globuleWEB.com
Fondation Max van Berchem | Avenue de Miremont 5 | CH-1206 Genève | Tél. / Fax : +41 22 347 88 91

redpajama_set_name: RedPajamaCommonCrawl


Enjoying artistic freedom afforded only an elite few, Fedde Le Grand is a masterful pioneer of electronica, considered by countless fans and artists as one of the single most defining figures in house music. Whether as DJ or producer, Fedde le Grand 's influence can be felt throughout the electronic landscape; his creative beats, grooves, melodies and rhythms surround us.
Back in 2006, it was the seminal electro track 'Put Your Hands Up For Detroit' that not only brought Fedde le Grand to global attention, but breathed fresh life into a stagnant house scene. Dubbed by many as the "Saviour of House", it soon became evident that the Dutchman was no one-trick pony. Amongst others, tracks like 'Let Me Think About It', 'Control Room', 'Sparks', his remixes of Coldplay's 'Paradise' and EBTG's 'Missing', 'The Creeps', 'So Much Love', 'Metrum', 'Autosave', 'Back & Forth', 'RAW' and lastly his amazing remix for Nikki Williams' 'Glowing' have established him as one of the most exciting and consistent talents around, demonstrating his effortless ability to move seamlessly between huge mainstream success and edgier, underground sounds. His 2009 debut artist album 'Output' was released in an incredible 64 countries worldwide, establishing him as one of the foremost creative forces in electronic music, while 2011 saw him accomplish a record-breaking 5 Beatport #1 tracks – including his reworking of 'Paradise' which earned him an opening set for Chris Martin's super-band in Madrid. Increasingly in demand for his remix skills, Fedde's talents have been called upon by a host of musical superstars, including Madonna, Coldplay and Robbie Williams to Will.i.am, Moby and Fatboy Slim.
Not only indulging in his own perfectionist musical tendencies, Fedde le Grand also nurtures new talent through his Flamingo imprint, using his years of hard-earned experience to push them towards superstardom. Nicky Romero, Deniz Koyu and Danny Avila are just some of the fledging talents that Fedde has already helped explode into the mainstream, and 2013 looks set to continue the trend with unknown artists set to breakthrough under Fedde's guiding hand.
Outside of the studio and around the globe hundreds of thousands have witnessed show-stopping live sets that explode with ingenuity and originality. Huge performances across continents are par for the course for Fedde le Grand, with the likes of Coachella, Exit Festival, Global Gathering, Electric Zoo, Mysteryland, Tomorrowland, Electric Daisy Carnival, Future Music and many more firmly under his belt. His residency at London's Ministry of Sound has become renowned as a world-class showcase of electro and house, continually selling out to roadblock crowds; his set at Ultra Music Festival 2012 was widely hailed as the best across the mammoth weekend, and to add a final much-lauded feather to his already crammed cap, he holds the coveted position as global headline resident for the jaw-dropping Sensation parties.
In 2012 Fedde le Grand announced the expansion of his critically-acclaimed Dark Light Sessions radio show from its birthplace in the US on broadcasting behemoth SiriusXM to stations across the planet, with countries as far spread as Brazil, Australia, Germany, New Zealand, Poland, Romania, Russia and more now receiving his blistering 60 minute mix on a weekly basis, earning Fedde le Grand an increasing hold on major dance music markets around the world.
Yet through all the success – the international chart-topping heights and global DJ fame – Fedde le Grand focus is simply fixed on making and playing great tracks. His dedication to music and his unwavering passion for the dancefloor continue to make him an intrinsic and dominant part of the ever-evolving electronic scene. A touchstone, an inspiration and a pioneer; he is definitive, he is essential, he is house music at its finest. He is Fedde Le Grand.


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text:
'Not Thinking About the Circus, at the Circus' by Angela Gardner
on Sep 11, 2016 August 19, 2021
'I write as a way of understanding'- Angela Gardner
Not Thinking About the Circus, at the Circus
I am shiny, towing an absence of sound through a tunnel. Holding
wrappers of the world I've arranged with head dead and disengaged
as tumble and throw subside. High wire step through the empty ring
of the moon. Its four quarters quartered inside, arms strength,
arm grasp, spin, climb and fall.
………………………………….AA door slams, a body slams.
It's important to rebuff distraction. Self-violence works on the body
with near misses, forcing confidences to strangers: that gift
of unburdening. I listen: her in tangles of herself sometimes messy.
And it all looks fine to start with: doll-witted within a thing, within
an overbalance. It's an edge she licks, for its bloody taste, hidden
from any clean-up crew.
A hard surface, oh yes but then there is ballast that sweetens the acts
in icing sugar. Access is a problem. She knows he sees what he sees,
in a dismount, to kiss or breathe.
……………………………………….IIt all hangs on the tethered wrist
or ankle: The idea of the real, companion to that personal copy we each
separately hold. That interval between possible worlds, the hinge
it all hangs from.
-Angela Gardner
Z.T.: Tell me about the way you write and what themes are particularly important to you.
A.G.::I write as a way of understanding and there is plenty to puzzle about! My main subjects in recent years have been the interaction of human and the natural world either with nature/culture (pastoral) or eco-poetic concerns. I'm also interested in science in particular the interface between biological and synthetic intelligence, but really because I'm trying to understand human consciousness and I love the language of these disciplines. But a number of poems come in response to visual art or theatre. I always take a notebook to exhibitions or will sit in the dark scribbling while, I watch physical theatre and modern circus. I just went to see Bangarra's latest work and it felt odd to have lost my notebook (temporarily) and not [to] be writing while watching.
Z.T.: I'm interest in your work at the intersection between poetry and visual art. How has it developed, where has it taken you and who have you collaborated with?
A.G.: I trained in visual arts in Wales, then at Queensland College of Art, and my practice now revolves around drawing, printmaking and artist's books. I work on collaborative artist's books with [the] NightLadder Collective and am in group shows with them. At the end of September, I go to Ottawa on a travel bursary to be part of a panel discussion regarding artist's books at Library and Archives Canada. I'm really looking forward to being able to attend the opening of the exhibition Open Books, that I have a work in, and also having time while I am over there to start another book of words and watercolour drawings. I have a number of collaborations with artists Caren Florance and Nicci Haynes which sees me go down to Canberra at least once a year. Caren is currently using a poem of mine Pleasure/Demolition as the basis for an artwork.
I keep up a correspondence with poet G.C. Waldrep (USA) and we will often recommend poets and poetry to each other. Whenever I am in London, I go to exhibitions with poet and art critic, Cherry Smith and Laurie Duggan, the Australian poet currently living in Kent (UK). There was a period of a few years when I caught the same train as Nathan Shepherdson and we would use the journey to talk poetry and art (his father is the painter, Gordon Shepherdson so, he is quite immersed in the world of visual art).
Z.T: What inspired you most about the Café Poet program and how did your residency at GOMA affect your poetry?
A.G.: I was inspired to become a Cafe poet because I really wanted to hang out in an art gallery. Who wouldn't, they are amazing places! I completed an ekphrastic poem, 'Unplanned Centaur' that was published in my latest Shearsman collection, The Told World, [with] research in GOMA's behind the scenes library. Lisa Gorton also selected 'The View from GOMA' for The Best Australian Poetry 2012 anthology. I mostly hung out in the cafe writing but there were some great exhibitions on at The Queensland Art Gallery and the Gallery of Modern Art while I was there so I got to have some really in-depth time with the artworks. The residency at GOMA also led to another opportunity as Australian Historical Society's artist in residence for their 'Conflict in History' project supported by UQ Art Museum and the School of History, Philosophy, Religion and Classic.
Z.T: You've published the thirteen issues of foame:e! What have you achieved so far and where do you want to take foam:e in the future?
A.G.: The online poetry journal foam:e (www.foame.org) … submissions window [is currently open, from] September to November. This year Carmen Keates is joining me to share the editorship. It's a chance to work with people (Jonathan Hadwen has just finished a three-year stint) and to really think about what is happening in poetry in Australia through interviews, reviews and poems. I'd like to see more women send in their work, the scales are tipped towards the men in submissions and that has showed some years in what we publish. It's an annual publication, so it is part of the rhythm of the year but it's always a thrill to find a new poet starting out and be able to publish their work among more established voices. I'd like foam:e to publish a print anthology sometime – poems from the back catalogue but also new, invited poems from contributors.
Angela Gardner
Angela Gardener's first poetry collection, Parts of Speech (UQP, 2007) won the Thomas Shapcott Arts Queensland Poetry Prize in 2006. Her most recent collections are The Told World (selected poetry) Shearsman Books UK and Thing & Unthing, Vagabond Press, Sydney both 2014. She is also a visual artist and edits at http://www.foame.org/. Angela Gardner was an Australian Poetry Cafe Poet in Residence at QAG/GOMA (Queensland Art Gallery/Gallery of Modern Art) in 2013.
Submissions to foam:e are by email addressed to foame.editor@gmail.com from 1 September to 30 November 2016. Include up to six poems in the body of the email and the name of the journal, foam:e in the subject line.
Read foame:e issue 13
More about Angela Gardner
Featured Writers Part 2: Past Australian Café Poets- Curated by Zalehah Turner
Read about the Australian Poetry Café Poet Program (2009-2014)
Zalehah Turner is a Sydney based critic, writer and poet currently completing her Bachelor of Arts in Communications majoring in writing and cultural studies at the University of Technology, Sydney. Zalehah is an Associate Editor of Rochford Street Review: https://rochfordstreetreview.com/2016/02/09/welcome-zalehah-turner-rochford-street-review-associate-editor
Previous: Teasing Threads – Sundry Film and Literary Criticism: Woody Allen's 'You Will Meet a Tall Dark Stranger'
Next: Luciano Prisco – New Works, Poems from Christopher Barnett: Mark Roberts on Christopher Barnett, Poetry and Collaboration.
Pingback: Australian Poetry's Cafe Poet Program (2009-2014) and contributing Café Poet bios (curated by Zalehah Turner) | Rochford Street Review
Pingback: Issue 19: July 2016 – September 2016 | Rochford Street Review


text:
ABC Orders The Wonder Years Reboot, Hip-Hop Drama Queens, More to Series
By Dave Nemetz / May 14 2021, 1:30 PM PDT
The Rookie, A Million Little Things and 3 Other Series Renewed at ABC
black-ish to End With Season 8 at ABC
ABC is filling out next season's primetime schedule, starting with an old favorite.
A reboot of The Wonder Years from executive producer Lee Daniels earned one of four series orders handed out by the Alphabet network on Friday, TVLine has learned. Like the original 1988-93 series, the Wonder Years reboot is set during the turbulent 1960s, but this time, it follows a Black middle-class family in Montgomery, Alabama through the eyes of 12-year-old Dean (Elisha "EJ" Williams). Dule Hill (Psych) and Saycon Sengbloh (In the Dark) play parents Bill and Lillian, and Laura Kariuki (Black Lightning) plays Dean's sister Kim; Don Cheadle (Black Monday) narrates the series as an grown-up Dean.
Also ordered to series at ABC: the drama Queens, which centers on four women now in their 40s who formed a hip-hop group together in the '90s. They "reunite for a chance to recapture their fame and regain the swagger they had" back in the day, per the official description. Eve (Eve), Brandy (Moesha), Naturi Naughton (Power) and Nadine Velazquez (My Name Is Earl) star as the foursome, with Taylor Selé and Pepi Sonuga (Famous in Love) co-starring. Scandal writer Zahir McGhee serves as series creator and EP.
Plus, ABC has ordered two comedies to series: Maggie and Abbott Elementary. Maggie stars Rebecca Rittenhouse (The Mindy Project) as a psychic who's trying to make sense of her own life. "Maggie regularly sees the fate of her friends, parents, clients, and random strangers on the street," the official synopsis says, "but when she suddenly sees a glimpse of her own future, Maggie is forced to start living in her own present." David Del Rio (The Baker and the Beauty), Nichole Sakura (Superstore) and Angelique Cabral (Life in Pieces) co-star; Justin Adler and Maggie Mull (Life in Pieces) are the co-creators as well as EPs.
Abbott Elementary is led by star/creator Quinta Brunson (A Black Lady Sketch Show) and is set at a Philadelphia public school. The workplace comedy follows the school's dedicated teachers and tone-deaf principal as they work hard to help their students succeed at life. Tyler James Williams (The Walking Dead), Janelle James, Chris Perfetti (In the Dark), Lisa Ann Walter (Emeril) and Sheryl Lee Ralph (Ray Donovan) also star.
As for the other pilots in consideration at ABC: The network hasn't yet decided the fates of dramas Epic, National Parks Investigation, Dark Horse, Promised Land and Triage, and they "will be considered at a later date for midseason." Meanwhile, comedies Adopted, Black Don't Crack and Bucktown and drama Acts of Crime are not moving forward.
TAGS: Abbott Elementary, ABC, Maggie, Queens, The Wonder Years
GET MORE: Series Orders
Berlin Film Festival Line-Up: Hong Sang-soo, Claire Denis…


text:
HSC 3030
HSC 3030 Week 5 Assignment 2 Policy Advocacy Presentation Latest Guide
Model:Recent
Analyzed and identified a clear policy position.
Analyzed and selected the appropriate audience to present the policy in front of.
Summarized the background information defining the problem being addressed in the proposed policy statement.
Analyzed and proposed a policy change, a new policy, or provide arguments against a proposed piece of legislation.
Analyzed and explained the intended beneficiaries of the policy and eligibility requirements.
Outlined the budgetary issues related to the proposed policy.
Analyzed and developed a closing argument summarizing a statement in support or against the policy issue.
Analyzed and included 15-20 slides.


text:
\section{Introduction}
\label{intro}

Processes of quenching star formation in galaxies can be divided into two
categories: internal and external. The latter, or environmental quenching, is
believed to be the primary mechanism of quenching galaxies with stellar masses
(${\rm M_{*}}$) lower than $10^{9.5}$${\rm\,M_\odot}$\ (or low-mass galaxies). Evidence of it
has been obtained at various cosmic epochs
\citep[e.g.,][]{peng10,peng12,geha12,wetzel13,
wheeler14,fillingham15,joshualee15,balogh16,fossati17,ycguo17dwarfenv,nancy17,woo17,ji18,papovich18}.
\citet{peng10} showed that environmental and internal (mass) quenching is
separable in the local universe and the importance of environmental (plus
merger) quenching overtakes that of mass (internal) quenching around
$10^{10}$${\rm\,M_\odot}$. \citet[][]{ycguo17dwarfenv} used the projected distance
($d_{proj}$) of a galaxy to its nearest massive neighbor with
${\rm M_{*}}$$>10^{10.5}$${\rm\,M_\odot}$\ as the indicator of environmental quenching and found
that low-mass quenched galaxies (QGs) have systematically smaller $d_{proj}$\ than
star-forming galaxies (SFGs), consistent with the scenario that if
environmental effects are significantly responsible for quenching low-mass
galaxies, QGs should live preferentially within a massive dark matter halo and
hence close to a massive central galaxy. A question, however, remains to be
more thoroughly studied: what is the role that internal processes play in the
quenching of low-mass galaxies?

To answer this question, an effective indicator of internal processes is
needed. Studies of massive galaxies suggest that central mass surface density
within the central radius of 1 kpc ($\Sigma_1$) is such an indicator.
\citet{cheung12} found that high $\Sigma_1$\ is the best predictor of quenching
at $z \sim 0.7$.  \citet{fang13} found that for nearby SDSS galaxies, specific
star formation rate (sSFR) varies systematically relative to $\Sigma_1$,
suggesting a mass-dependent threshold of $\Sigma_1$\ for the onset of quenching,
possibly due to a threshold in black hole mass. \citet{vandokkum14},
\citet{tacchella15a}, and \citet{barro17} extended the use of $\Sigma_1$\ as a
quenching indicator to higher redshifts.  Since massive galaxies are primarily
quenched by internal processes
\citep[e.g.][]{darvish15,darvish16,lin16,delucia19}, $\Sigma_1$\ hence can be
treated as an indicator of internal quenching. Moreover, \citet{terrazas16b}
found that quiescence is strongly correlated with black hole mass in central
galaxies, suggesting that $\Sigma_1$\ is very likely a proxy of black hole mass.
\citet{chen20} proposed a model to correlate $\Sigma_1$\ with the mass of
supermassive black holes. Recently, \citet{luo20} correlated $\Sigma_1$\ with
the bulge types in nearby galaxies.

In this paper, we use $\Sigma_1$\ to explore quenching in low-mass galaxies.
Comparing the $\Sigma_1$\ of QGs and SFGs would reveal clues on the quenching
mechanisms. \citet{woo17} studied the $\Sigma_1$\ between SFGs and QGs in SDSS
galaxies, and found that in all environments, at a given ${\rm M_{*}}$, QGs have a
0.2-0.3 dex higher $\Sigma_1$\ than SFGs. They argued that either $\Sigma_1$\
increases subsequent to satellite quenching, or the $\Sigma_1$\ for individual
galaxies remains unchanged, but the ${\rm M_{*}}$\ of galaxies at the time of
quenching is significantly different from those in the green valley. Their
sample is down to ${\rm M_{*}}$=$10^{9.75}$${\rm\,M_\odot}$, just around the ${\rm M_{*}}$, where the
quenching mechanisms are believed to change. Currently, however, similar
studies are lacking for low-mass galaxies beyond the local universe. We will
use the CANDELS data to explore lower-mass regime at $z \geq 0.5$.

The physical meaning of $\Sigma_1$\ in low-mass and massive galaxies, however,
is different. The choice of 1 kpc, which is limited by the spatial resolution
of HST/WFC3, is reasonably small for massive galaxies to sample their central
region, but it is quite close to the effective radius of low-mass galaxies,
raising a concern of its validity to represent the central region. Galaxies,
however, extend well beyond their half-light radius. \citet{mowla19} showed
that the 80\%-light radius ($r_{80}$, i.e., the radius containing 80\% of the
total galaxy light) of low-mass galaxies at $z \lesssim 1.5$ is about 5 kpc,
and this radius increases insignificantly from $10^9$${\rm\,M_\odot}$\ to
$10^{10.5}$${\rm\,M_\odot}$.  \citet{miller19} showed that the difference in $r_{80}$
between SFGs and QGs is small. Based on these results, we presume that,
although $\Sigma_1$\ might not represent the core density of low-mass galaxies
as it does for massive galaxies, it is still a very good indicator of the mass
surface density in the inner region of galaxies below $10^{10.5}$${\rm\,M_\odot}$.
Therefore, as long as we compare galaxies with similar total ${\rm M_{*}}$, using
$\Sigma_1$\ to study the change of inner mass density before and after quenching
is valid and in fact very important to connect the density change to quenching.

In this paper, we adopt a flat ${\rm \Lambda CDM}$ cosmology with
$\Omega_m=0.3$, $\Omega_{\Lambda}=0.7$, and the Hubble constant $H_0 = 70\ {\rm
km~s^{-1}~Mpc^{-1}}$. We use the AB magnitude scale \citep{oke74} and a
\citet{chabrier03} initial mass function.

\section{Data, Sample, and $\Sigma_1$} \label{data}

We identify QGs and SFGs from CANDELS \citep{candelsoverview,candelshst}
through sSFR. We start from the multi-wavelength photometry catalogs of four
CANDELS fields: COSMOS \citep{nayyeri17cosmos}, EGS \citep{stefanon17egs},
GOODS-S \citep{ycguo13goodss}, and UDS \citep{galametz13uds}.  Photometric
redshifts and ${\rm M_{*}}$\ were measured by \citet{dahlen13} and \citet{santini15}.
Basically, for each galaxy, 10 investigators ran their spectral energy
distribution (SED)-fitting codes on the galaxy \citep[see Table 1
of][]{santini15}. They were free to choose their preferred star formation
histories ($\tau$-model, constant, delayed, inverse $\tau$, etc.) and many
other free parameters. Nine of them used Calzetti law \citep{calzetti00} to
account for dust extinction. Each investigator delivered the best-fit
parameters (including ${\rm M_{*}}$\ and star formation rate [SFR]).
We then took the median of the 10 results as the ``team consensus'' parameters
of the galaxy. We believe that this method, used in many CANDELS papers, is
able to reduce the uncertainties and systematics of each individual code or
parameter choices used in SED fitting.

$\Sigma_1$\ used in this paper is the same as that used in \citet{chen20}.  It
is calculated in three steps. First, we run FAST \citep{kriek09fast} on
multi-aperture photometry of CANDELS galaxies \citep{liufs16,liufs18} to
measure ${\rm M_{*}}$\ within each aperture, and then derive the mass density within
the central 1 kpc. This $\Sigma_1$\ is the observed (point spread function
(PSF)-smoothed) $\Sigma_1$. Because of the PSF effect, this observed $\Sigma_1$\
is smaller than the intrinsic one.  Next, we calculate a model $\Sigma_1$\ by
using the {S\'{e}rsic}\ model of each galaxy \citep{vanderwel12}. We measure the
model H-band band flux within 1 kpc and convert it into ${\rm M_{*}}$\ with the best
SED-fit mass-to-light ratio. This $\Sigma_1$\ is the model $\Sigma_1$. Last, for
galaxies at a given redshift, we derive an average relation between the
difference in the observed and model $\Sigma_1$\ (defined as the observed minus
model) as a function of the {S\'{e}rsic}\ index ($n$). This relation reveals the
average mass difference caused by the PSF effect, which is then added to the
observed $\Sigma_1$\ at a given redshift and $n$. This hybrid method largely
corrects for PSF effects and central deviation from {S\'{e}rsic}\ models, providing
a reliable measurement of the intrinsic $\Sigma_1$. {The magnitude of our PSF
correction and its effect on the observed results of $\Sigma_1$\ are shown in
Appendix A.} Our $\Sigma_1$\ agrees excellently with others in the literature
\citep[e.g.,][]{barro17}.

Our $\Sigma_1$\ measurement is primarily based on aperture photometry, and the
use of {S\'{e}rsic}\ models is only to correct for the PSF effect. The accuracy of
the {S\'{e}rsic}\ model plays a role in our derived correction and hence in our
measurement. The correction is derived from the average difference of a
population of galaxies. Therefore, for a population of galaxies, as long as
their average {S\'{e}rsic}\ measurement is not biased by systematic errors, our
method is reasonable to recover their average (mean or median) $\Sigma_1$. In
our later analysis, we only use the mean or median $\Sigma_1$\ of a given
population to draw our conclusion. \citet{vanderwel12} showed that for
low-{S\'{e}rsic}\ index galaxies ($n < 3$) or for small galaxies (effective radius
$r_e < $0.3$^{\prime\prime}$), the systematic error of the {S\'{e}rsic}\ index measured from
CANDLES F160W is almost zero (a relative error of 0.02 for $n < 3$ and 0.00 for
$r_e < $0.3$^{\prime\prime}$) down to an F160W magnitude of 25 AB (see their Table 3).
Low-mass galaxies in our study are indeed galaxies with low $n$ or small $r_e$.
Therefore, based on our scientific objective (i.e., understanding the average
behavior of quenched low-mass galaxies), we are able to use the CANDELS F160W
{S\'{e}rsic}\ measurements to F160W mag = 25 AB.

\begin{figure}[htbp]
\hspace*{-0.5cm}
\includegraphics[scale=0.23, angle=0]{sigma1_hudf_test_nore.ps}

\caption[]{Comparison of $\Sigma_1$\ in regions with different depths (indicated
by F160W image's root-mean square error RMS) in CANDELS/GOODS-S. Galaxies are
divided into star forming (blue) and quenched (red). For each galaxy, its
$\Sigma_1$\ is compared to the median of galaxies in the Deep region (Region II)
with the same redshift, ${\rm M_{*}}$, and star formation activity (star forming or
quenched). The difference (individual minus the median) is the $\Sigma_1$\
deviation in the Y-axis. Squares (and diamonds) with error bars show the
3$\sigma$ clipped mean and standard deviation of the mean for quenched (and
star-forming) galaxies. The four regions are: the Hubble Ultra Deep Field
(HUDF, I), Deep (II), Wide (III), and Edge (IV) based on the RMS value of the
F160W image at the location of the galaxies. The smaller the RMS, the deeper
the survey.

\label{fig:hudftest}} \end{figure}

We further test the effect of survey depth on the accuracy of $\Sigma_1$. We
separate galaxies in GOODS-S into regions of the Hubble Ultra Deep Field
(HUDF), Deep, Wide, and Edge (which is for edge or corner regions where the
depth is very shallow due to the drizzle pattern). The survey depth varies
across a range of more than 2.5 mag from the HUDF to the Edge. We choose the
Deep region as our fiducial region due to its decent depth and large number of
galaxies. For each galaxy in any region, we compare its $\Sigma_1$\ to the
median $\Sigma_1$\ of galaxies in the Deep region with the same redshift,
${\rm M_{*}}$, and star formation activity (star forming or quenched). The difference
(or $\Sigma_1$\ deviation) is shown in Figure \ref{fig:hudftest}. We find no
obvious difference between the four regions (the largest deviation is that QGs
in the Edge region is about 0.07 dex lower than the other three regions).
Moreover, we find no obvious trend of the deviation changes with the survey
depth. This test provides strong evidence that if limited to F160W = 25 AB,
even though most of CANDELS regions are shallower than HUDF, our $\Sigma_1$\
measurement has little systematic biases to a population of galaxies regardless
of survey depth. {The result in Figure \ref{fig:hudftest} shows the statistics
of the whole sample. To specifically test the robustness of our $\Sigma_1$\
measurement in low-mass galaxies, we repeat it for a subsample of low-mass
galaxies with ${\rm 10^{8.5} < M_*/M_\odot < 10^{9.5}}$ at $0.5<z<1.0$. The new
result, shown in Appendix A, indicates again no significant systematic
deviations found between QGs and SFGs across the four survey depths.}

We therefore limit our low-mass sample to sources with F160W $H\leq25$ AB, no
suspicious F160W photometry, SExtractor CLASS\_STAR$<$0.8, and a clean {S\'{e}rsic}\
fit flag in \citet{vanderwel12}. To study its corresponding mass limit, we use
two stellar population models. The first one represents young galaxies with a
constant star formation history and an age of 0.5 Gyr. The second represents
old galaxies with a single starburst right after the big bang. This model has
the maximum age that a galaxy can have at a given redshift. We then normalize
the two models to have the F160W magnitude of 25 AB. The old model (with a high
mass-to-light ratio) corresponds to a much higher stellar mass than the young
one (Figure \ref{fig:sample}). We therefore choose the old one as our mass
limit at different redshifts. As a sanity check, we also use the empirical
formula derived by \citet{chartab20} to measure the mass-complete limit of
F160W = 25 AB \footnote{The formula of mass limit in \citet{chartab20} is for
F160W = 26 AB. We renormalize their formula to match F160W = 25 AB.}. Their
formula is derived by following the method of \citet{pozzetti10}, which is a
common practice in measuring stellar mass functions for large surveys. The
empirical limit matches very well with our model limit at $0.5 \leq z < 2.5$.
We therefore determine that our mass limit is $10^{9.2}$${\rm\,M_\odot}$\ at $0.5 \leq z
<1.0$, $10^{9.6}$${\rm\,M_\odot}$\ at $1.0 \leq z <1.5$, and $10^{10.0}$${\rm\,M_\odot}$\ at $1.5
\leq z < 2.5$ (the three large dotted rectangles in Figure \ref{fig:sample}).
To push our mass limit even lower, we also include galaxies with ${\rm M_{*}}$\
between $10^{8.8}$${\rm\,M_\odot}$\ and $10^{9.2}$${\rm\,M_\odot}$\ at $0.5 \leq z < 0.7$, where our
sample is also mass complete (the smallest dotted rectangle in Figure
\ref{fig:sample}).

\begin{figure}[htbp] \includegraphics[scale=0.15,
angle=0]{envsig_9panel_stat_2_sample_H25.ps}

\caption[]{Sample selection. CANDELS galaxies of $0.5 \leq z < 2.5$ with F160W
H $\leq$ 25 AB are shown as gray points. QGs between $10^{8.8}$ and
$10^{11.2}$${\rm\,M_\odot}$\ are red. The three curves show different estimations of mass
completeness of H $\leq$ 25 AB as described in text. The four blue dotted
rectangles show our mass-complete sample of QGs at different redshifts.

\label{fig:sample}} \end{figure}

\begin{figure*}[htbp]
\includegraphics[scale=0.23, angle=0]{ssfrvssigma1_2_25.0.ps}

\caption[]{sSFR as a function of $\Sigma_1$\ in different redshift and ${\rm M_{*}}$\
bins. In each bin, galaxies are divided into SFGs (black) and QGs (red). The
horizontal solid and dotted purple lines are the 3$\sigma$ clipped mean sSFR
and its 3$\sigma$ deviation for galaxies in the bin. The vertical solid and
dashed black (and brown) lines are the 3$\sigma$ clipped mean $\Sigma_1$\ and
the standard deviation of the mean of $\Sigma_1$\ of SFGs (and QGs). The QG
samples in shaded panels are mass incomplete (SFGs are mass complete, though).
The four panels toward the bottom left with thick borders highlight the main
result of this paper.

\label{fig:ssfrvssigma1}}
\end{figure*}

\section{Results} \label{results}

\subsection{Difference of $\Sigma_1$\ between QGs and SFGs} \label{results:diff}

Figure \ref{fig:ssfrvssigma1} shows the sSFR as a function of $\Sigma_1$\ in
different redshift and ${\rm M_{*}}$\ bins. In each bin, first, for galaxies with sSFR
$> 10^{-2} / Gyr$, we calculate the 3$\sigma$ clipped mean and standard
deviation of the mean of sSFRs (purple solid and dotted lines). Galaxies with
an sSFR lower than $-3\sigma$ (the lower dotted line) are classified as QGs,
while the others are classified as SFGs. Our mean sSFR and its scatter
($\sigma$) are consistent with those in the literature
\citep[e.g.,][]{whitaker14,kurczynski16}.

Figure \ref{fig:ssfrvssigma1} shows that, for almost all redshift and ${\rm M_{*}}$\
bins, the 3$\sigma$ clipped mean $\Sigma_1$\ of QGs (solid vertical brown lines)
is greater than that of SFGs (solid vertical black lines). Figure
\ref{fig:stat} shows the statistics.

For massive galaxies (${\rm M_{*}}$$\geq 10^{10}$${\rm\,M_\odot}$), at all redshifts, the mean
$\Sigma_1$\ of QGs is significantly ($\gtrsim 10 \sigma$) larger than that of
SFGs with the same redshift and ${\rm M_{*}}$\ (Panel (b) of Figure \ref{fig:stat}).
The difference decreases with ${\rm M_{*}}$. This result is consistent with many other
studies at various redshifts
\citep[e.g.,][]{cheung12,fang13,vandokkum14,barro17,chen20}. This difference in
$\Sigma_1$, combined with no difference in $d_{proj}$\ between massive QGs and SFGs
found in \citet{ycguo17dwarfenv}, demonstrates that internal processes,
especially those related to central mass density, e.g., possibly black holes,
are the primary way to quench massive galaxies from $z=2.5$ to $z=0.5$
\citep[e.g.,][]{chen20} or even to today \citep[e.g.,][]{luo20}.

The new, interesting result is the $\Sigma_1$\ comparison in the low-mass regime
(i.e., panels highlighted by thick borders in Figure \ref{fig:ssfrvssigma1}).
At ${\rm M_{*}}$$\lesssim 10^{9.5}$${\rm\,M_\odot}$\, we find a $\gtrsim$0.3 dex difference with
very high statistical significance ($\gtrsim 5\sigma$) between the mean
$\Sigma_1$\ of QGs and SFGs at $z<1.5$. This result suggests that quenching has
a relation with the increase of $\Sigma_1$\ in low-mass galaxies, similar to the
situation of massive galaxies reported by many studies. We will discuss its
implications in detail in Section \ref{discussion}.

To remove the mass dependence of $\Sigma_1$\ further, we calculate the ratio
between $\Sigma_1$\ and ${\rm M_{*}}$\ of galaxies (called mass-normalized $\Sigma_1$,
which is proportional to the fraction of total ${\rm M_{*}}$\ within the central 1kpc
radius, but differs by a factor of $\pi$). As shown in Panel (c) of Figure
\ref{fig:stat}, this mass-normalized $\Sigma_1$\ decreases with ${\rm M_{*}}$\ for
massive QGs. Our trend matches the slope (dashed line) derived through the
best-fit $\Sigma_1$--${\rm M_{*}}$\ relation of QGs from \citet{barro17}. For low-mass
galaxies at $z<1.0$, our QG trend shows a turnover at $10^{10}$${\rm\,M_\odot}$, and
decreases with the decreasing of ${\rm M_{*}}$. This turnover is mainly a reflection
of changes in the {S\'{e}rsic}\ index ($n$) and size (see Figure 13 of
\citet{barro17}). For $n \sim 4$ galaxies, the mass-normalized $\Sigma_1$\
decreases when galaxy size increases. Massive QGs have $n \sim 4$ and their
size increases with ${\rm M_{*}}$. Therefore, their mass-normalized $\Sigma_1$\
decreases with ${\rm M_{*}}$. However, for low-mass QGs at $z \leq 1.0$, their size is
flattened in the ${\rm M_{*}}$--size diagram \citep[e.g.,][]{vanderwel14size}.
Moreover, their $n$ gradually changes from $\sim 4$ to $\sim 1$ with the
decrease of ${\rm M_{*}}$. The combination of the two (constant size and decreasing
$n$) makes their mass-normalized $\Sigma_1$\ decreases moderately from the peak
at $10^{10}$${\rm\,M_\odot}$\ and approach a constant value of -1.1 dex. This turnover at
$10^{10}$${\rm\,M_\odot}$\ is also around the stellar mass where quenching mechanisms
gradually changes from being dominated by internal processes to by external
processes
\cite[e.g.,][]{peng10,cybulski14,joshualee15,darvish15,darvish16,wetzel15a,balogh16,fillingham16,lin16,ycguo17dwarfenv,lee18}.

\begin{figure}[htbp]
\hspace*{-0.3cm}\includegraphics[scale=0.12,
angle=0]{sigma1_stat_4new_25.0.ps}

\caption[]{Statistics of $\Sigma_1$. In each panel, different redshifts are
shown by different symbols, and different types of galaxies are shown by
different colors. Panel (a) shows the 3$\sigma$ clipped mean of $\Sigma_1$\ as a
function of ${\rm M_{*}}$. Panel (b) shows the difference between the 3$\sigma$
clipped mean of $\Sigma_1$\ of SFGs and QGs ($\Delta$ = QG - SFG). Panel (c)
shows the mass-normalized $\Sigma_1$\ as a function of ${\rm M_{*}}$. The dashed line
shows the slope derived from \citet{barro17}. Panel (d) is similar to Panel
(b), but showing the difference between the mass-normalized $\Sigma_1$\ of SFGs
and QGs. In each Panel, symbols connected by lines are mass complete in our
sample, while those not connected are mass incomplete.

\label{fig:stat}}
\end{figure}

\begin{figure}[htbp]
\hspace*{-0.3cm}\includegraphics[scale=0.12,
angle=0]{ssfrvssigma1_stack_25.0_lowz4.ps}

\caption[]{Relations between different parameters and the residual Log(sSFR) of
galaxies at $0.5 \leq z < 1.0$. The residual Log(sSFR), or $\Delta$Log(sSFR),
is defined as the difference between the Log(sSFR) of a galaxy and the average
Log(sSFR) of galaxies on the star-forming main sequence at the same redshift
and ${\rm M_{*}}$\ of the galaxy. Namely, the zero-point of $\Delta$Log(sSFR)
corresponds to the solid horizontal purple lines in Figure
\ref{fig:ssfrvssigma1}. The four panels show (a) $\Sigma_1$, (b) mass-normalized
$\Sigma_1$\ (i.e., Log($\Sigma_1$/$M_*$), (c) semi-major axis, and (d) {S\'{e}rsic}\
index. In each panel, galaxies are divided into four ${\rm M_{*}}$\ bins, as the
labels of different colors show. The curves and error bars show the mean and
the standard deviation of the mean (both after 3$\sigma$ clipping) of each
${\rm M_{*}}$\ bin. The three vertical black lines show the boundaries of three
regions, as indicated in Panel (c): star forming (SF), green valley (GV), and
quenched (Q).

\label{fig:lowzstat}}
\end{figure}

\begin{figure}[htbp]
\hspace*{-0.3cm}\includegraphics[scale=0.12,
angle=0]{ssfrvssigma1_stack_25.0_lowz3.ps}

\caption[]{Similar to Figure \ref{fig:lowzstat_delta}, but using the residual
values (rather than their exact values) for the parameters in the Y-axis. The
residual of a parameter is defined as the difference between the parameter of a
galaxy and the average of galaxies on the star-forming main sequence at the
same redshift and ${\rm M_{*}}$\ of the galaxy. For example, $\Delta$Log($\Sigma_1$) is
defined by using the solid vertical black lines in Figure
\ref{fig:ssfrvssigma1} as the zero-point.

\label{fig:lowzstat_delta}}
\end{figure}

The mass-normalized $\Sigma_1$\ of SFGs is almost a constant across a wide range
of ${\rm M_{*}}$, and is lower than that of their QG counterparts. The difference of
mass-normalized $\Sigma_1$\ between the two populations (Panel (d) of Figure
\ref{fig:stat}) is very similar to that of $\Sigma_1$\ (Panel (b)). The trend of
the mass-normalized $\Sigma_1$\ of massive SFGs is still uncertain in the
literature. For example, \citet{barro17} found a sublinear slope (0.88) for the
$\Sigma_1$--${\rm M_{*}}$\ relation, which turns into a mass-normalized $\Sigma_1$\
slightly decreasing with ${\rm M_{*}}$. \citet{chen20} revisited this issue and found
a superlinear slope (1.1) for the $\Sigma_1$--${\rm M_{*}}$\ relation, which implies
the mass-normalized $\Sigma_1$\ slightly increases with ${\rm M_{*}}$. Overall, both
slopes are quite close to 1, implying a close-to-flat trend of mass-normalized
$\Sigma_1$. Therefore, our result of an almost constant trend does not
significantly different from either slope.

\subsection{$\Sigma_1$\ and Structural Parameters vs. sSFR} \label{results:delta}

An efficient way to investigate the overall behavior of galaxies over a wide
range of parameter space is to use the ``residual'' plot
\citep[e.g.,][]{barro17,woo17,fang18,chen20,lin20}. Instead of showing the
exact values of a parameter, this type of plot shows the relative values of the
parameter with respect to a common value, for example, the mean or median of a
sample. By taking into account of the different mean or median values of
different samples, this method enables a direct comparison between them.

We use the residual plot to show the relations between some parameters and the
sSFR. In Figure \ref{fig:lowzstat}, we only use the residual for the sSFR in
the X-axis, but still keep the exact values of other parameters in the Y-axis
for readers who are interested in the exact values. In Figure
\ref{fig:lowzstat_delta}, we use the residual for both axes to compare
different subsamples with different ${\rm M_{*}}$. The zero-point of the residual is
calculated by the average value of galaxies in the star-forming main sequence
at a given ($z$, ${\rm M_{*}}$) bin. For example, the zero-point of  $\Delta$Log(sSFR)
(or $\Delta$Log($\Sigma_1$)) is the solid horizontal purple lines (or solid
vertical black lines) in Figure \ref{fig:ssfrvssigma1}. Hereinafter, we only
focus on the redshift range of $0.5 \leq z < 1.0$. We also divide galaxies into
three categories based on their ${\rm M_{*}}$: low-mass (Log(${\rm M_{*}}$)$<9.6$),
intermediate-mass ($9.6 \leq $Log(${\rm M_{*}}$)$<10.4$), and massive ($10.4
\leq$Log(${\rm M_{*}}$)$< 11.2$).

To catch the transition between SFGs and QGs, we divide galaxies into three
(rather than previous two) types based on their $\Delta$Log(sSFR): star forming
(SF), green valley (GV\footnote{To be accurate, this type should be called
``transition''. We use ``GV'' simply to follow the naming scheme in studies of
massive galaxies.  There is no evidence yet to show there is a ``valley'' in
between SFGs and QGs in the distributions of low-mass galaxies at $z>0.5$.}),
and quenched (Q). The divisions are shown in Panel (c) of Figure
\ref{fig:lowzstat} and \ref{fig:lowzstat_delta}. They are quite similar to
those used in \citet{woo17,liufs18,chen20}. In SF, $\Sigma_1$\ and
$\Sigma_1$/${\rm M_{*}}$ of galaxies of all ${\rm M_{*}}$\ changes little (Panel (a) and (b)
of both figures). In GV, all galaxies increases their $\Sigma_1$\ (or
Log($\Sigma_1$/${\rm M_{*}}$)) dramatically by about 0.2-0.3 dex. The increase of
$\Sigma_1$\ of massive galaxies during GV has been discussed in \citet[][see
their Figure 5]{chen20}.  Our result shows that intermediate- and low-mass
galaxies also follow a similar trend during GV. In Q, galaxies with different
${\rm M_{*}}$\ show a slight difference. Massive galaxies reach a plateau of about 0.3
dex in $\Delta$Log($\Sigma_1$) or $\Delta$Log($\Sigma_1/M_*$). This plateau is a
reflection of the vertical part of the ``elbow'' shape in the panels of massive
galaxies in Figure \ref{fig:ssfrvssigma1}. This trend and its meaning on
quenching have been thoroughly discussed by \citet{barro17}, \citet{woo17}, and
\citet{chen20}. On the other hand, intermediate- and low-mass galaxies continue
to grow their $\Sigma_1$ after GV. This trend is especially true for
intermediate-mass galaxies, and less obvious for low-mass galaxies due to large
uncertainties of small number statistics.

The relation between Log($\Sigma_1$) (or $\Delta$Log($\Sigma_1$)) and
$\Delta$Log(sSFR) is correlated with the change of other structural parameters
of galaxies. Panel (c) and (d) of Figure \ref{fig:lowzstat} and
\ref{fig:lowzstat_delta} show the change of size (semimajor axis) and the
{S\'{e}rsic}\ index ($n$). In GV and Q, the sizes of galaxies decrease with
$\Delta$Log(sSFR). Low-mass and massive galaxies have a similar decreasing
trend, while intermediate-mass galaxies decrease faster. Although
intermediate-mass galaxies are larger than low-mass ones in SF, because of this
faster decrease, their size approach the size of low-mass galaxies when
$\Delta$Log(sSFR) is very low (Panel (c) of Figure \ref{fig:lowzstat}). This
result is consistent with the flattened curve of the size--mass relation of QGs
in the low-mass regime \citep[e.g.,][]{vanderwel14size}.

Low-mass galaxies and massive galaxies, however, have different trends of $n$.
Low-mass galaxies start with a disk-like shape ($n=1$) in SF, then mildly
increase $n$ in GV and Q, and finally to reach $n \sim 2$ -- still disk-like --
in the end of Q. Massive galaxies already start with $n \sim 2$ in SF and
quickly increase $n$ during GV and the beginning of Q to $n \sim 4$
(spheroid-like) and remain around $n \sim 4$ in Q. Intermediate-mass galaxies
lie between the two extremes. Overall, to summarize, massive galaxies' plateau
of Log($\Sigma_1$) at $\Delta$Log(sSFR)$<-2$ correlates with (almost) no change
in size and $n$ in Q. Low-mass galaxies' increasing $\Sigma_1$\ in Q correlates
with a gradual increase of $n$ more than with a slight decrease of size.
Intermediate-mass galaxies' increasing $\Sigma_1$\ in Q, on the other hand,
correlates more with a dramatic decrease of size.

\section{Discussion} \label{discussion}

The main result of this study is the difference between the mean $\Sigma_1$\ of
QGs and SFGs in the low-mass regime (${\rm M_{*}}$$\lesssim10^{9.5}$${\rm\,M_\odot}$) at
$z\sim1$. Similar results have also been reported in the local universe for
galaxies with ${\rm M_{*}}$$>10^{9.75}$${\rm\,M_\odot}$\ in \citet{woo17}. Here, we discuss some
implications of this result for the quenching processes of low-mass galaxies.
Although the real quenching processes are very likely to be complicated and
complex, our discussions are still useful to place some constraints on
quenching and environmental effects.

When we discuss $\Sigma_1$\ and quenching, it would be very useful to separate
low-mass central and satellite galaxies \footnote{See, however, a series of
papers by \citet{wangenci18a,wangenci18b,wangenci20}. They showed that the
separation of central and satellite galaxies is not as fundamental as using
galaxy ${\rm M_{*}}$\ in discussing quenching mechanisms, because the quenching
properties (e.g., bulge-to-total-light ratio, central velocity dispersion, and
prevalence of optical/radio-loud active galactic nuclei (AGN), etc.) of central
and satellite galaxies are quite similar as long as both stellar mass and halo
mass are controlled. An earlier work by \citet{ycguo09cen} also found similar
structural parameter distributions between central and satellite galaxies when
mass and color are controlled.}. As shown in \citet{woo17}, $\Sigma_1$\ of the
transition galaxies (i.e. green-valley galaxies) decreases smoothly with the
environment by as much as 0.2 dex for ${\rm M_{*}}$=$10^{9.75}-10^{10}$${\rm\,M_\odot}$\ galaxies
from the field, large halo-centric distance, to small halo-centric distance in
SDSS. In our sample, however, due to the limitation of using photometric
redshift, galaxy clusters or groups cannot be accurately identified. In
\citet{ycguo17dwarfenv}, we found that the median projected distance
($d_{proj}$) from low-mass ($M_* \lesssim 10^{9.5}$${\rm\,M_\odot}$) QGs to their massive
($M_* \gtrsim 10^{10.5}$${\rm\,M_\odot}$) neighbors is systematically smaller than that of
low-mass SFGs. Also, \citet{ycguo17dwarfenv} showed that $\sim90\%$ of low-mass
QGs are within 2 times the virial radius of their neighboring massive halos.
These results suggest that (1) on average, low-mass QGs are found closer to
massive central galaxies (i.e., higher density region) than low-mass SFGs and
(2) most of low-mass QGs tend to be satellite galaxies. Therefore, the results
we see in Figure \ref{fig:ssfrvssigma1} -- \ref{fig:lowzstat_delta} are likely
driven by satellite galaxies.

In next two subsections, we interpret the curves in Figure \ref{fig:lowzstat}
and \ref{fig:lowzstat_delta} as evolutionary tracks. This interpretation is not
necessarily true, especially when progenitor bias is considered (Section
\ref{discussion:bias}). It is, however, still reasonable and useful for our
discussion when the change of ${\rm M_{*}}$\ of galaxies is small, which is likely
true when galaxies quench. The decrease of sSFR results in a moderate increase
of ${\rm M_{*}}$, which then keeps most galaxies within their initial ${\rm M_{*}}$\ bins, as
shown in Figure \ref{fig:lowzstat} and \ref{fig:lowzstat_delta}.

\subsection{Low-mass Galaxies in Green Valley} \label{discussion:gv}

$\Sigma_1$\ of low-mass galaxies increases by about 0.25 dex in GV, indicating
that the quenching mechanisms (possibly environmental effects) gradually quench
star formation in an outside-in process, i.e., preferentially removing gas from
outskirts of galaxies while maintaining their central star formation to
increase $\Sigma_1$. We can use the growth of total ${\rm M_{*}}$\ and $\Sigma_1$\ to
estimate the timescale of galaxies in GV. We will use the sSFR gradient of
low-mass transition galaxies reported in \citet{liufs18} as our constraint.

We consider a galaxy entering GV with ${\rm M_{*}}$\ of $10^{9.2}$${\rm\,M_\odot}$\ at $z<1.0$.
Its sSFR (and hence SFR) can be measured from our sample and is -0.5 dex below
the average Log(sSFR) of star-forming main sequence (as defined in Figure
\ref{fig:lowzstat}). When this galaxy exits GV, its sSFR drops by another -0.75
dex to reach -1.25 dex below the star-forming main sequence. Now, we assume
this galaxy spends $T_{GV}$=1, 2, and 4 Gyr in GV. Its Log(sSFR) drops linearly
with time over this period (i.e., sSFR drops exponentially). Since the change
of sSFR is only -0.75 dex, very small compared to the whole sSFR range from SF
to Q, the exact form of the decreasing is not important.

For each time step of 0.1 Gyr in GV, based on the galaxy's current ${\rm M_{*}}$\ and
sSFR, we calculate its ${\rm M_{*}}$\ and sSFR for the next step. From its new ${\rm M_{*}}$,
we infer its new $\Sigma_1$\ from Panel (b) of Figure \ref{fig:lowzstat} (or
\ref{fig:lowzstat_delta}). Based on the change in ${\rm M_{*}}$\ and $\Sigma_1$\ in
this step, we calculate the SFR (and sSFR) within and outside the central 1
kpc. We repeat this process until the galaxy exits GV. The results are shown in
Figure \ref{fig:gv}.

\begin{figure}[htbp]
\hspace*{-0.3cm}
\vspace*{-0.3cm}
\includegraphics[scale=0.12,angle=0]{massevol_gv.ps}

\caption[]{Growth of a galaxy in GV in our simple models (see Section 4.1). The
four panels show (a) ${\rm M_{*}}$, (b) $\Sigma_1$, (c) sSFR, and (d) SFR,
respectively. In each panel, different line styles show assumptions of
different time the galaxy spends in GV, as indicated in Panel (b). In Panel (c)
and (d), we also show the curves for the regions within (and outside) the
central 1 kpc in red (and blue).  The green hatched region in Panel (c) shows
the defined GV.

\label{fig:gv}}
\end{figure}

We use two conditions to constrain $T_{GV}$: (1) SFR within central 1 kpc
should not exceed the total SFR and (2) the difference between sSFRs within and
outside central 1 kpc should match the observed sSFR gradient in
\citet{liufs18}, which has a difference of about 0.3 dex within and outside the
central 1 kpc (see their Figure 5). The first condition indicates that a small
$T_{GV}$ is unlikely.  In the case of $T_{GV}$= 1 Gyr (dotted lines in Figure
\ref{fig:gv}), the central SFR exceeds the total SFR in a few hundred million
years (compare red and black dotted lines in Panel (d)). The short timescale
requires an unrealistically high SFR in the center to boost $\Sigma_1$. The case
of $T_{GV}$= 2 Gyr meets the first condition, but fails the second one. The
difference between the central and outer sSFR is $\gtrsim$0.5 dex (red and blue
dashed lines in Panel (c)), which is larger than the observed sSFR difference
in \citet{liufs18}. The case of $T_{GV}$=4 Gyr meets both conditions and is
therefore most likely to be true.  $T_{GV}$ longer than 4 Gyr would produce a
much smaller difference between central and outer sSFRs, inconsistent with the
observed sSFR gradient in \citet{liufs18}.

Our (rough) estimate of $T_{GV}$ suggests that the time a low-mass galaxy
spending on GV is about a few gigayears. If we define this time as the
quenching timescale (i.e., time for transitioning from star forming to
quenched), our value here is consistent with the quenching timescale estimated
by using the dynamics and spatial distribution of quenched low-mass galaxies in
large halos in \citet{ycguo17dwarfenv}. It is also consistent with the estimate
of the quenching timescale of galaxies around $10^{9.5} M_\odot$ in
\citet{balogh16} and \citet{fossati17}. \citet{ji18} also estimated a quenching
timescale of a few gigayears ($\sim$4 Gyr) by using the redshift evolution of
the clustering strength of CANDELS galaxies. Similarly, \citet{phillipps19}
found timescales for galaxies crossing GV at lower redshifts $0.1 < z < 0.2$ is
also a few gigayears (2-4 Gyr). Overall, the quenching of low-mass galaxies is
not rapid, but rather a gradual and long processes. The quenching timescale can
be used to test quenching mechanisms, which need to, not only reduce the total
and outskirt SFR by a factor of 3 in a few gigayears, but also maintain the
central (within 1 kpc) SFR almost constant over this long period (see solid
lines in Panel (d) of Figure \ref{fig:gv}).

The long quenching timescale of low-mass galaxies is consistent with the low
quenching efficiency measured in many studies. For example, \citet{nancy17},
\citet{papovich18}, and \citet{chartab20} all found that the environmental
quenching efficiency decreases with the decrease of ${\rm M_{*}}$. The mass quenching
efficiency also decreases with the decrease of ${\rm M_{*}}$\
\citep[e.g.,][]{chartab20}. Both efficiencies are quite low at
${\rm M_{*}}$$<10^{9.5}$${\rm\,M_\odot}$\ \citep{nancy17,chartab20,contini20}. Therefore, the
quenching timescale is expected to be long.

One model to explain the quenching of low-mass galaxies involves both
``starvation'' (i.e., cutting off gas supplies by environmental effects
\citep[e.g.,][]{larson80,balogh97}) and ``overconsumption'' (i.e., gas
depletion because of star formation and star-formation driven outflows
\citep{mcgee14}). The gas depletion time is shorter at high redshifts when SFR
is higher, but increases with the cosmic time. In fact, the gas depletion time
for GV galaxies at $z<1.0$ is about a few gigayears \citep[inferred
from][]{genzel15}, consistent with our estimate of the quenching timescale. In
a recent paper, \citet{trussler20} found that quenching is driven by both
starvation and outflow, and they estimated the quenching timescale is a few to
several gigayears (depending on the models) in the local universe.
\citet{moutard18}, however, argued for a delayed-then-rapid quenching scenario
\citep{wetzel13}, where quenching of low-mass galaxies is rapid (a few hundred
megayears) after a long period since entering high-density regions.

The long quenching timescale also allows GV galaxies to transform their
morphology while quenching their star formation in gradual processes.
\citet{nancy17} found that the morphologies of lower-mass QGs are inconsistent
with those expected of recently quenched SFGs. Our results are consistent with
their conclusion, as both $\Sigma_1$\ and the {S\'{e}rsic}\ index ($n$, although only
mildly) increase when low-mass galaxies evolve from SF to GV, and eventually to
Q, as shown in Figure \ref{fig:lowzstat}. \citet{nancy17} argued that simple
gas removal processes, e.g., strangulation and ram pressure, are not able to
transform morphology and therefore some dynamical processes need to be
involved, e.g., galaxy interactions, tidal stripping, and disk fading. Our
results, however, suggest that the long star formation duration ($\sim 4$ Gyr)
in central region is able to increase $\Sigma_1$\ and $n$.

\subsection{Low-mass Galaxies after Green Valley} \label{discussion:after}

Once a low-mass galaxy exits GV, its total sSFR drops to at least -1.25 dex
lower than the star-forming main sequence, and is therefore too low to form
many new stars to effectively increase its total ${\rm M_{*}}$. Its $\Sigma_1$,
however, still increases.  For example, when the galaxy we discuss in Figure
\ref{fig:gv} exits GV after 4 Gyr, its ${\rm M_{*}}$=$10^{9.4}$${\rm\,M_\odot}$, and its
Log($\Sigma_1$) is 8.25 (solid black lines in Panel (a) and (b)). From the blue
curve of Panel (b) of Figure \ref{fig:lowzstat}, we know that galaxies with
similar ${\rm M_{*}}$\ would have Log($\Sigma_1$/${\rm M_{*}}$) of -0.95 in the end of Q (the
blue curve at $\Delta$Log(sSFR)$<-2$), corresponding to a $\Sigma_1$\ of 8.45.
Therefore, its $\Sigma_1$\ increases by 0.2 dex in Q. Since few new stars are
formed in this period, the galaxy cannot increase its $\Sigma_1$\ by star
formation.

Therefore, $\Sigma_1$\ has to be increased by some environmental effects through
the redistribution of existing stars. Most effects, e.g., harassment and tidal
stripping, tend to make satellite galaxies more extended rather than more
concentrated while reducing their overall ${\rm M_{*}}$\
\citep[e.g.,][]{carleton19,tremmel19}. A scenario, however, is possible to
effectively ``increase'' $\Sigma_1$: if harassment or tidal stripping only
remove outskirt stars of a galaxy while keeping its center intact, the galaxy
will keep the same $\Sigma_1$\ but move to lower ${\rm M_{*}}$, equivalent to
increasing its $\Sigma_1$/${\rm M_{*}}$\ \citep[see][and references therein]{woo17}. In
our example above, to match the observed Log($\Sigma_1$/${\rm M_{*}}$)$\sim$-0.95 at
$\Delta$Log(sSFR)$<$-3 in Q, the galaxy needs to lose about 30\%-40\%
($\sim$0.2 dex) of its ${\rm M_{*}}$\ after exiting GV.

The mass loss of satellite halos due to environmental effects is well studied.
For example, \citet{jiang16} showed that a $10^{11}$${\rm\,M_\odot}$\ halo orbiting a
$10^{13}$${\rm\,M_\odot}$\ halo loses half its mass in about 2.5 Gyr. \citet{lee18} also
show that if subject to tidal stripping of a massive neighboring halo, halos
around $10^{11}$${\rm\,M_\odot}$\ often lose a large fraction ($> 20\%$) of their peak
mass. The fraction of the lost halo mass seems to match the required ${\rm M_{*}}$\
loss discussed above, but satellite galaxies lose halo mass more easily than
losing ${\rm M_{*}}$. As shown in \citet{engler21}, the ${\rm M_{*}}$--${\rm M_{halo}}$\ relation of
satellite galaxies is higher than that of central galaxies. Therefore, once
becoming a satellite, a galaxy would lose a much higher fraction of its initial
halo mass than the fraction of its initial ${\rm M_{*}}$. As inferred from
\citet{errani18}, the loss of $\sim$50\% of halo mass is only corresponding to
the loss of a few percents of ${\rm M_{*}}$, much lower than the needed 30\%--40\%
discussed above.  In order to lose 30\%--40\% of ${\rm M_{*}}$, satellite halos need
to lose $\gtrsim 90\%$ of their halo mass, which seems too high to be true.

\subsection{Progenitor Bias}
\label{discussion:bias}

One alternative explanation of the ``increase'' of $\Sigma_1$\ in Q is
progenitor bias. It is used to explain some observed redshift evolution of
galaxy properties, e.g., the size of massive QGs
\citep[e.g.,][]{belli15,keating15,shankar15} and  the increase of massive QGs'
$\Sigma_1$\ with redshift \citep{tacchella17}. In the redshift evolution of QGs'
size--mass relation, newly quenched systems have larger sizes and therefore
increase the average size of the quenched pool toward low redshifts.

Similarly, progenitor bias suggests that low-mass galaxies with the highest
$\Sigma_1$\ at low redshifts are quenched at higher redshifts, when galaxies
have higher surface mass densities. These earlier quenched systems increases
the average $\Sigma_1$\ of the quenched pool at low redshifts when comparing it
to low-redshift SFGs. This explanation is possible, as high-redshift QGs have
higher $\Sigma_1$\ than low-redshift QGs at the same ${\rm M_{*}}$\ (Figure
\ref{fig:stat}). It, however, has another requirement: high-redshift low-mass
QGs need to have higher $\Sigma_1$\ than their SFG counterparts. Low-mass SFGs
(down to $10^{9}$${\rm\,M_\odot}$) in our highest-redshift bin $1.5 \leq z < 2.5$ (where
our sample is still mass-complete, as shown in Figure \ref{fig:sample}) have a
lower $\Sigma_1$\ than QGs in our lowest-redshift bin ($0.5 \leq z < 1.0$).
Therefore, if low-mass QGs at $z\sim2$ have a similar average $\Sigma_1$\ as
low-mass SFGs at $z\sim2$, they are not able to explain the higher end of
$\Sigma_1$\ of the low-redshift low-mass QGs.  High-redshift low-mass QGs need
to have a $\sim$0.4-0.5 dex higher $\Sigma_1$\ than their SFGs counterparts to
validate the explanation.

There are two ways to satisfy this requirement. First, only SFGs with the
highest $\Sigma_1$\ are able to quench. At ${\rm M_{*}}$$\sim$$10^{9}$${\rm\,M_\odot}$, the
highest Log($\Sigma_1$) of SFGs at $z\sim2$ is $>$8.5 (see the shaded panels in
Figure \ref{fig:ssfrvssigma1}). This value is high enough to explain the
high-end of $\Sigma_1$\ around ${\rm M_{*}}$$\sim$$10^{9}$${\rm\,M_\odot}$\ at $z<1.0$. This way
implies that high $\Sigma_1$\ at high redshifts is a direct indicator of
quenching and therefore that internal quenching could be important for low-mass
galaxies at high redshifts. The second way is that high-redshift low-mass
galaxies also undergo the dramatic growth of $\Sigma_1$\ in GV, similar to what
we discussed in Section \ref{discussion:gv}. The second way is preferred,
because we do see a range of $\Sigma_1$\ in high-redshift low-mass QGs from
Figure \ref{fig:ssfrvssigma1} (even with a mass-incomplete sample), which is
inconsistent with the assumption of the first way that only the low-mass SFGs
with the highest $\Sigma_1$\ at $z\sim2$ are able to quench.

A few further observations can test the progenitor bias in low-mass galaxies.
(1) A mass-complete sample at high redshift and low mass is needed to test the
difference in $\Sigma_1$\ between SFGs and QGs. (2) The number density of QGs at
high redshifts (and with high $\Sigma_1$) should match that of QGs with the
highest $\Sigma_1$\ in low redshift. (3) $\Sigma_1$ should correlates with the
age of stellar population of QGs. Namely, the higher the $\Sigma_1$, the older
the QGs.

\subsection{Similarity and Difference between Low-mass and Massive Galaxies}
\label{discussion:diff}

An interesting and intriguing result of our study is the similarity between
low-mass ($\lesssim 10^{9.5}M_\odot$) and massive ($\gtrsim 10^{10.4}M_\odot$)
galaxies at $0.5 \leq z < 1.0$ in the relation between $\Delta$Log($\Sigma_1$)
(or $\Delta$Log($\Sigma_1$/${\rm M_{*}}$)) and $\Delta$Log(sSFR) (see Panel (a) and (b)
of Figure \ref{fig:lowzstat_delta}). This similarity is especially true for the
dramatic increase of $\Sigma_1$\ in GV.

As discussed in Section \ref{intro}, $\Sigma_1$\ has been shown to be an
effective indicator of internal quenching of massive galaxies\footnote{See,
however, \citet{lilly16} for a different explanation of $\Sigma_1$. They argued
that the higher $\Sigma_1$\ is a consequence rather than the cause of quenching.
See also \citet{chen20} for more discussions of this explanation.}, possibly
correlated with supermassive black hole mass. \citet{chen20} found that for
massive galaxies, most black hole mass growth takes place in GV. If low-mass
galaxies are a scale-down of massive galaxies, the physical processes that
build up black hole mass and $\Sigma_1$\ and that provide feedback from high
$\Sigma_1$\ in massive galaxies could also work in low-mass galaxies.

In fact, recent studies found evidence of a central engine to provide feedback
in low-mass galaxies. \citet{bradford18} found deficiencies of HI gas in
isolated AGN-host low-mass galaxies, suggesting that black hole feedback or
shocks from extreme starburst destroy or consume the cold gas. Stellar feedback
(related with central starburst) has been considered to be a major effect for
low-mass galaxies, since the fraction of AGN hosts decreases with ${\rm M_{*}}$, and
so does the importance of black hole/AGN feedback
\citep[see][though]{kaviraj19}.  However, a large sample of low-mass galaxies
have been found to have signatures of black holes \citep{reines13,reines15},
providing the sources of the central engines of quenching. \citet{greene20}
suggested that a high fraction of $10^9-10^{10} M_\odot$ galaxies hosting
intermediate-mass black holes.  \citet{penny18} found evidence for AGN feedback
in a subset of 69 quenched low-mass galaxies (in groups) in the MANGA survey.
Their result demonstrates the importance of AGN feedback in maintaining
quiescence of low-mass galaxies.

A few differences, however, exist between low-mass and massive galaxies. First,
as we discussed in Introduction, the physical meaning of $\Sigma_1$\ may be
different for the two populations. In massive galaxies, $\Sigma_1$\ samples well
the core mass surface density, while in low-mass galaxies, it represents more
the inner density within a large portion of the effective radius. Second,
low-mass QGs do not have a classical bulge, while massive galaxies do. This
difference is evident by the {S\'{e}rsic}\ index of both populations ($n \sim 2$ for
low-mass QGs and $n \sim 4$ for massive QGs, as shown in Panel (d) of Figure
\ref{fig:lowzstat}).  Last, low-mass SFGs and QGs are found to have different
projected distances to massive galaxies \citep{ycguo17dwarfenv}, indicating
different impacts of environmental effects.

The role of the increased $\Sigma_1$\ in low-mass galaxies could be a
``preprocessing'' of quenching. \citet{socolovsky19} found that in dense
environments at $z < 1$, compact low-mass SFGs (which would have a higher
$\Sigma_1$\ at a given ${\rm M_{*}}$) are preferentially quenched. They proposed that
both strong feedback and environmental effects act together to quickly quench
them. By stacking spectra of high-sSFR galaxies, they even found that more
compact galaxies are more likely to host outflows. Their results are broadly
consistent with ours, both indicating that low-mass galaxies with high
$\Sigma_1$\ are more easily to be quenched than those with a low $\Sigma_1$\ when
they fall into a dense environment. \citet{ycguo16bursty} showed that the star
formation history of low-mass galaxies is bursty at $z\gtrsim1$. Star formation
can {\it temporarily} quench these galaxies, but new gas accretion and
recycling induce new episodes of starburst. To fully quench them, some effects,
potentially environmental, are required to turn off the continuous gas supply.

\section{Summary}
\label{summary}

We use CANDELS data to study the relationship between the central stellar mass
surface density ($\Sigma_1$) and quenching of low-mass galaxies at $0.5 \leq z <
1.5$,
Our mass-complete sample allows us to investigate galaxies down to $\sim
10^9$${\rm\,M_\odot}$\ at $0.5 \leq z < 1.0$ with reliable $\Sigma_1$\ measurements. At a
given redshift and ${\rm M_{*}}$\ bin, we compare the mean $\Sigma_1$\ of QGs and SFGs.
We find that for massive (${\rm M_{*}}$\ $>10^{10}$${\rm\,M_\odot}$) galaxies, QGs have
significantly higher average $\Sigma_1$\ than SFGs, consistent with other
studies in the literature.  Intriguingly, we find that low-mass QGs also have
a higher $\Sigma_1$\ than low-mass SFGs at $z\sim1$. At $z \leq 1.0$, the
difference of $\Sigma_1$\ between QGs and SFGs increases slightly with ${\rm M_{*}}$\
at $\lesssim 10^{10}$${\rm\,M_\odot}$\ and then decreases with ${\rm M_{*}}$\ for more massive
galaxies.

We use $\Delta$Log(sSFR), namely, the difference between galaxies' Log(sSFR)
and that of the star-forming main sequence at the same $z$ and ${\rm M_{*}}$, to
further divide galaxies into three categories: SF, GV, and Q. At $0.5 \leq z <
1.0$, we find that the $\Sigma_1$\ of galaxies increases dramatically in GV, by
about 0.25 dex, regardless of their ${\rm M_{*}}$. In Q, massive galaxies reach a
plateau in $\Sigma_1$, which correlates with (almost) no change of size and $n$.
Low-mass galaxies' increasing $\Sigma_1$\ in Q correlates more with a gradual
increase of $n$, while intermediate-mass galaxies' increasing $\Sigma_1$\ in Q
correlates more with a dramatic decrease of size.

We use the growth of ${\rm M_{*}}$\ and $\Sigma_1$\ of low-mass galaxies in GV to
constrain their time spent in GV. By matching the observed sSFR gradient in
\citet{liufs18}, we estimate that the quenching timescale of low-mass galaxies
is a few ($\sim4$) Gyr at $z<1.0$. Quenching mechanisms need to gradually
quench star formation in an outside-in way, i.e., preferentially removing gas
from outskirts of galaxies while maintaining their central star formation to
increase $\Sigma_1$. In Q, the increase of $\Sigma_1$\ in low-mass QGs is still
unknown, with possible explanations including dynamical processes and/or
progenitor bias.

We also discuss the similarity and difference between low-mass and massive
galaxies. Although environmental effects are believed to dominate the quenching
of low-mass galaxies, the similar trend of $\Delta$Log($\Sigma_1$) vs.
$\Delta$Log(sSFR) suggests that internal processes in quenching low-mass
galaxies should also be investigated. Future studies can improve our
understanding in a few aspects: (1) using a mass-complete sample to explore
low-mass galaxies at higher redshifts and (2) investigating black holes/AGN in
low-mass galaxies and their relation to galaxy properties (e.g., central mass
density) in all environments.

\

The authors thank the anonymous referee for providing valuable comments, which
improved the manuscript. Support for Program number HST-AR-13891, HST-AR-15025,
and HST-GO-12060 were provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities for
Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Members of
the CANDELS team at UCSC acknowledge support from NASA HST grant GO-12060.10-A
and from NSF grants AST-0808133 and AST-1615730. SL acknowledges the support
from the National Research Foundation of Korea (NRF) grant
(2020R1I1A1A01060310) funded by the Korean government (MSIP).

{

redpajama_set_name: RedPajamaArXiv


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Feathers, Fuddles and Hope. What!?
Feathers: They are soft, they drift and can wander wherever, in my world they are a wonderment, they represent Part to Whole with their collective pieces helping a bird to fly, often times very pretty, possibly colorful, full of potential-representing dreams and hopes, and they are floaty-a fun word and a fine flexible attribute!
I have been thinking about connectivity, the occurrences that happen and the randomness (or not) of it all. The never-ending question of…Are their Coincidences? Do all things happen for a reason, however unclear it may be at the time?
Fuddles, a character in my children's picture book, is a protagonist with the cause being the Wonder of Planet Earth. Fuddles image became a feather from the seed of an idea that "something" could impart "goodness." The form that the something was to take began with conversations and bouncing around ideas. I needed a physical form but I couldn't get my finger on. Once Fuddles was a feather it all became clear. Fuddles was not only an ecological presence but also one of hope and vision. Months later I came to realize the strong connection to the hope concepts of Fuddles. Hope became a topic of much thought and conversation with many who crossed my path. In this (not so random) universe the topic of hope seems to be everywhere these days. (Or is that just my awareness and focus?) From the somewhat benign, such as the weather forecast which can't get enough of the omnipresence Hope for (the upcoming and not soon enough for me) Spring, to the paramount news reminding us this is the anniversary of the famous Edmund Pettus Bridge walk in Selma Ala. where Hope was, and still is, a clear message. I randomly was watching a movie called Finding Normal that stated, "…and now these three remain: faith, hope and love. But, the greatest of these is love." (apparently that is a biblical passage from Corinthians 13:13.) So there is was again, this time in entertainment. We all know the idiom of-Hope springs eternal. Indeed, Hope is sometimes the string that keeps us moving foreword in large and small endeavors.
I looked up the symbolic meanings of feathers and found this. "Symbol meaning of feathers deal with ascension and spiritual evolution to a higher plane…Native American Chiefs wore feathers to symbolize their communication with Spirit, and to express their celestial wisdom…Another symbol meaning of feathers also revolves around prayer, and the Pueblo use feather sticks as they dance in prayer for rain during solstice rituals..As a Celtic symbol meaning (connected the Druids to) sky gods and (to) gain knowledge of the celestial realm…The Egyptians believed that feathers were symbolic of sky gods too. Ma'at, the Egyptian goddess of justice, would weigh the hearts of the newly dead in the underworld against the weight of a feather to determine the worthiness of his or her soul…In Christianity feathers represented virtues. In fact, an image of three feathers were made into signet rings – each feather symbolizing Charity, hope, and faith…In dreams feathers meanings point to travel or the ability to move more freely in life. White feathers in dreams indicate innocence or a fresh start in a spiritual sense." -(read more –website) All the above are essentially about Hope. Hope has a forward momentum, it's about the future and thinking thoughts/dreams/desires/needs as to what's next, regardless of how immediate or far off in the "next" may be.
My question to you is as follows. It's for further books and for my curiosity. What emotions, and words do feathers evoke for you?
The Original feather of inspiration.


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Topflight offer a range of unforgettable hillwalking holidays to some of the most beautiful mountain landscapes in Europe, experience a range of hiking trails and explore the most scenic routes with our wonderful collection of hillwalking holidays.
Topflight offer a range of unforgettable hiking holidays for your hillwalking group. We have many years of experience dealing with hiking, hillwalking and walking groups. We understand that each and every group is unique, so we will work with you to create the perfect itinerary to suit your needs and desires. Topflight are proud to be the preferred travel partner of Mountaineering Ireland. We offer a range of exclusive group benefits for you and your group. Tailormade itineraries, guided tours, exclusive accommodation, free group leader places and much more. The benefits your group will receive are unique to each trip.
We understand that not everybody wants to travel in a group, so we have created many Hillwalking Tours to suit the needs of individuals who love hiking. This wonderful tour has been specially designed to cater to the needs of solo travellers, allowing you to embark on the adventure of a lifetime with like-minded people. No single supplement applies. Experience an incredible seven night Singles Hillwalking Tour in Tirol, Austria.


Neat opportunity to locate your business in Richland Township along busy M89, just east of the Village of Richland. Building is a small office with an upper-level storage area that could be finished into additional office area. Property is immediately across from Richland Lanes bowling alley. Uses could include financial services, real estate, insurance, office-service users, contractors, plumbers, etc. Zoning offers many options for users. Sellers reserves two outbuildings and picket fence. Call listing agent with questions.


OH so much fun! LOve the embossed panel, Karren!
I just bought this stencil, and had no idea how much potential it has...your background is so striking, and it looks like black 'Patent Leather'! Beautiful Copic coloring on your images and fabulous take on the sketch! Such a fun card, Karren!
Oh, that shiny stencilling is just great, Karren and makes a beautiful bg on the black!!! Love your cute as can be little bunny with his lovely balloons!!! Such a sweet card - LOVE it!!!
WOW!!! seriously amazing card, karren!! love the translucent embossing paste and your perfect coloring!!
Ooo, I love the black on black texture! The bunny and balloons are colored so beautifully too. Thanks for joining us on the Simon Says Stamp Monday Challenge.


Hi everyone. A while ago I had a day where I tried out the Floating Alcohol Inks technique. I made lots of different combinations of colours, using leftover pieces of glossy card stock. Click HERE to see a card I posted earlier using one of those backgrounds. This technique produces a marbled look --- very cool!
Fast forward 9 months later ... I still have a big stash of these backgrounds. Just so happens that my good friend, Karen is running a challenge on Splitcoaststampers using this fun technique. Here's a link to Karen's Floating Alcohol Ink card.
Since I used a snippet of glossy to make my background, I'm heading over to Snippets Playground for some fun!
And dropping in to play at Simon Says Wednesday where Anything Goes this week.
what a great guy card - must get the alcohol inks out and have a go at this!
You make me want to go through my stash for colorful backgrounds and try something like this! Fantastic idea for them and fast too!
A great masculine card using theses techniques, Loll!
Very nice masculine card, Loll. You are always using different techniques. I know what you mean by using up some of the stash. I look through it once in a while. Does that count?
Haven't braved the world of Alcohol Inks as yet. Only just getting my feet wet on Brusho's and Water Colours!
Oh, your alcohol ink panel looks great, Loll - love the clocks and the colours - yeah for using some of the stash, hey - I don't really own a lot of alcohol inks, but I think I should give this technique a try!!!!! What a lovely masculine card card you created!!!
This is a very cool technique, Loll. How smart of you to have a stash of these panels.
Gorgeous Loll and yet another technique I want to try!!!
Your background looks great with the stenciled clock on top of it - a fabulous masculine card!
Such a cool technique!! I will definitely have to give this a try!
That looks so cool. Really has you looking at it and wondering "how'd she do that?". Glad I know now.
giggle....thanks so very much for the nod mf!! You rock!
I giggled because we really need to get together. I have sooooo many bkg. pieces in my stash that I need to find a use for. I make them and then don't know what I want to do with them.
I really like how this card turned out. The stencil over the hints of colour looks really great.
I was just telling Karen I need to have a Karen technique day and I should include you in that, Loll. You have so many unique ideas for using the techniques and this is a prime example.


text:
Ambassador Nipon welcomed the Governor of the Tourism Authority of Thailand
Mr. Nipon Petchpornprapas presented the Letter of Credence to H.E. Mr. Zoran Milanovic, President of the Republic of Croatia
Mr. Nipon Petchpornprapas presented the Letter of Credence to H.E. Dr. Vjosa Osmani-Sadrio, President of the Republic of Kosovo
The Royal Thai Embassy in Budapest organizes a seminar to educate Thai workers on their rights and duties under the Hungarian laws
Thai students participate in the International Chemistry Tournament 2022 in Hungary
Mr. Nipon Petchpornprapas presented the Letter of Credence to H.E. Ms. Katalin Novák, President of the Republic of Hungary, as Ambassador Extraordinary and Plenipotentiary of the Kingdom of Thailand to Hungary
On 2 June 2022, the Royal Thai Embassy in Budapest organized a ceremony to commemorate the auspicious occasion of Her Majesty Queen Suthida Bajrasudhabimalalakshana's Birthday Anniversary on 3 June 2022.
On 29 May 2022, the Royal Thai Embassy in Budapest participated in the Children's Day Celebration at Budapest City Park organized by International Children's Safety Service.
On 1 May 2022, Ms. Pilanya Niyomthai, Minister Counsellor, together with officials from the Royal Thai Embassy in Budapest, participated in the Thai New Year celebration (Songkran) organized by Thairattanaprateep Temple in Budapest


text:
NEWS-PHOTOS
MESSAGES OF THE RECTOR MAJOR
RMG - 27 August: Constantino Vendrame, 125th anniversary of birth of Servant of God
(ANS - Rome) - Costantino Vendrame was born in San Martino di Colle Umberto, in the diocese of Vittorio Veneto (Treviso) on 27 August 1893. His parents Pietro and Elena Fiori taught him to love work and sacrifice and above all the Lord. From an early age, Constantino distinguished himself by his intelligence and his goodness. He completed his high school studies in the seminary of Vittorio Veneto and in 1913 he put into practice his dream of becoming a Salesian and entered the novitiate of Ivrea.
After a first experience in the oratory of Chioggia, he was called to serve his country, participating in the First World War (1915-18) with other Salesian confreres who, like him, emerged from this harsh experience further tempered in body and spirit. Ordained priest in Milan, in March 1924, he received the missionary crucifix in Valdocco in October, in the Basilica of Mary Help of Christians, and on November 30 he left for India. On December 23 he is in Shillong, in Assam, a mountainous area to the north-east of India, under Tibet, on the border with China, between the Khasi and Yaintia tribes.
He had the task of approaching the area's inhabitants and in less than a year he was appointed parish priest of the city. Visiting the villages, reaching the "outskirts" via rough and tiring mountain paths, meeting families and children without distinction of ethnicity and religion, starting Salesian oratories to make Jesus and his Gospel known was his mission, one he lived by giving himself wholly for the glory of God and the salvation of souls until the very end of his life on January 30, 1957, at Dibrugarh. Near legendary not only the number of conversions and baptisms he administered, but also the fruit of his extraordinary mission that still continues to inspire amazement. Prayer was the secret of his strength, love for the Sacred Heart of Jesus and Mary Help of Christians the inspiration of all his works.
Both his native city and the Diocese of Vittorio Veneto cultivate a great devotion to their fellow countryman and promote the Cause of his Beatification that also involves the young and keeps alive the missionary zeal and the commitment to announce today the Gospel that so distinguished Fr Costantino.
ANS - "Agenzia iNfo Salesiana" is a on-line almost daily publication, the communication agency of the Salesian Congregation enrolled in the Press Register of the Tibunal of Rome as n 153/2007.
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