My Christmas stash is gone so needed to make some Christmas cards. When I saw this FREE image I thought it would make super cute cards and I have a friend that would love it! And I think my step-MIL will like this one too! One of my regulars needed a card for a friend of his and he didn't have anything in mind. So I thought this would work. I sent him a photo and his response was "can I have that one for my mom instead!" He said she loves Cardinals. So then I had to think of another card for his friend (see button Christmas tree). I added stickles to the snowflakes and snow mounds but the snowflake sparkle didn't show up very well. I used this card from Taylored Expressions as my inspiration.
1) December Inspirational Card Challenge @ Scrapbook.com – Lift Category – lift a card from Taylored Expressions blog or Pinterest.
2) December Scraplift your Favorites @ Scrapbook.com – Any Favorite. You can lift a favorite layout, a favorite card, a favorite sketch, a favorite project or whatever your favorites may be. It can be a favorite from anywhere (Pinterest, blog, scrapbook.com, etc).
Digital Stamp: Warm Winter Snow @ Free Dearie Dolls Digi Stamps (she has three versions with and without snow) My husband then worked his magic and made it a color version with no snow.
Accents/Tools: Darice snowflake embossing folder, Lawn Fawn Stitched Hillside Borders, Frosted Lace Stickles, EK Success 1/16 pop dots.
I had an order for a lady that works in NY but has a cabin she lives in when not working. She loves to go to cabin and enjoy nature. So when I found The Great Outdoors Kit (or cheaper version is Camping Kids) at Imagine That Digi Shop I knew it would be perfect. I added an extra tree to my scene. Pop dotted the fire wood stack, chair and the knobs sticking out on the actually cabin to make it feel more real. I still haven't quiet figured out how to make my grass longer than the die without leaving that little mark…if you know the secret please do tell. The lady loved it and has it displayed on her work desk to reminder her of "cabin life".
1) Creative Link Up @ Imagine That Creative Playground – make a card and link it up. If you use an Imagine That Digi then you get the stamp of the month for free.
My Godparents sent an email that their grandson's teacher sent out. She asked for Valentine cards to be sent to the child at school so they could learn about different places in the world. So I asked what he likes being 6 yoa and in 1st grade and was told dinosaurs, Pokemon and Star Wars. Mary Ellen drew some cute dinosaurs at Free Dearie Dolls Digi Stamps so I used one of them. I decided for the squares to use small version of the states that the card was coming from (Missouri) and going to (California). I used MOJOMonday #482 sketch but instead of a circle inside I went with a jagged edge square.
See next post for card without maps.
1) Feb Card Sketch Challenge @ Scrapbook.com – sketch #2.
2) Feb Inspirational Card Challenge – theme – love.
Images: free maps on internet, Valentine Boy T-rex @ Free Dearie Dolls Digital Images.
Since the dino is so cute and funny I decided he needed to be sent to my guy friend, Dale. I try to send Dale a card for each of the holidays…who doesn't need happy mail?!!
So I apparently put my paper in wrong in the embossing folder because the textured side go the indent embossing (not sure what that is called) so I decided to use it! I thought it worked great with getting the love/valentine theme across without being a lovey dovey card! I hope the dino makes him smile like it makes me!
Images: Valentine Boy T-rex @ Free Dearie Dolls Digital Images.
I used the colors from the May Inspirational Card Challenge – color category. I used MFTWSC182 sketch which was one of the sketches in last months April Inspirational Challenge. I used all scraps for this card.
1) May Inspirational Card Challenge – Color category.
So the lady at work wanted a card for her BFF whose husband has been injured and not healing. Been a long road but they finally found out he has something that keeps him from healing. There is no cure but they can manage it now that they know he has it. My co-worker wanted to encourage her friend during this time. She found the "hang in there" card I did for my friend and said she wanted something similar. This is what I came up with. I used MOJO Sketch #446 for my inspiration.
1) May Inspirational Card Challenge – Favorites Category – used a past MOJO sketch.
Inside: I hope you have the Happiest Valentine Day in all the Kingdom.
So a lady at work saw the princess birthday card I did and wanted a valentine one for her nieces. So I kept design same but placed a heart in the middle…tried to make it look like they were holding it. This is the last of the princess dies in the package so will have to make Christmas cards with the rest of the dies.
1) Feb Inspirational Card Challenge @ Scrapbook.com – favorites Category – sketch saved was Mojo Monday Sketch #433.
So this is my 2nd attempt at the sketch category on the Feb Inspirational Card Challenge @ Scrapbook.com. Got closer but still don't have the strip with sentiment on it.
I got to use my brand new embossing folder I got for my birthday. I made up wish list at stores on internet and my husband picked from them. This one is from Taylored Expressions. I also got to use up Valentine scraps for the striped paper. My goal was to try to use up from my scraps and most of my Valentine Cards this year were made from scraps!! Happy Dance!
2) Creative Playground Challenge #1: Show Us Your Heart.
3) Customer Link up at Imagine That…Digis by Kris – use a Imagine That digi and make a project. Once you have made 10 projects you will get a $6.00 code to the store. Here is my card #5.


text:
Alcohol/Entertainment & Late Night Refreshment
Club Premises Certificate
General information and guidance about Club Premises Certificates is available to download from this page. Other types of application form are available from the Licensing Section.
Why do I need a licence?
To authorise the supply of alcohol and regulated entertainment in a qualifying club you need a club premises certificate from your local authority.
In a qualifying club there is technically no sale by retail of alcohol (except to guests) as the member owns part of the alcohol stock and the money passing across the bar is merely a mechanism to preserve equity between members where one may consume more than another. In order to constitute a qualifying club you must also satisfy the various requirements set out in the Licensing Act 2003.
What will I have to do?
Clubs must be qualifying clubs. A qualifying club has general conditions it must satisfy. These are:
a person may not be given memberships or as a candidate for membership to any membership privileges without an interval of at least two days from their membership application or nomination and their membership granted
that club rules state that those becoming member without nomination or application cannot have membership privileges for at least two days between them becoming members and being admitted to the club
that the club is established and conducted in good faith
that the club has at least 25 members
that alcohol is only supplied to members on the premises on behalf or by the club
Additional conditions in relation to the supply of alcohol must be complied with. These conditions are:
that alcohol purchased for and supplied by the club is done by members of the club who are over 18 years of age and are elected to do so by members
that no person at the expense of the club receives any commission, percentage or other similar payment in regard to the purchase of alcohol by the club
that there are no arrangements for anyone to receive a financial benefit from supplying alcohol, apart from any benefit to the club or to any person indirectly from the supply giving a gain from running a club.
Registered industrial and provident societies and friendly societies will qualify if the alcohol is purchased for and supplied by the club is done under the control of members or a committee of members.
What does the application process involve?
A summary of the regulation relating to this licence is available as a link on this page.
What does the evaluation process involve?
A club can apply for a club premises certificate for any premises which are occupied and used regularly for club purposes.
Applications should be made to the local licensing authority, which will be the local authority where the premises are situated. Applications should be submitted with a plan of the premises which must be in a specific format, a copy of the rules of the club and a club operating schedule.
A club operating schedule is a document which must be in a specific format and includes information on:
the activities of the club
the times the activities are to take place
other opening times
if alcohol supplies are for consumption on or off the premises or both
the steps that the club propose to take to promote the licensing objectives
any other information that is required.
If there are any alterations to the rules or name of the club before an application is determined on or after a certificate is issued, the club secretary must give details to the local licensing authority. If a certificate is in place this must be sent to the licensing authority when they are notified.
If a certificate is in place and the registered address of the club changes the club must give notice to the local licensing authority when they are notified.
If a certificate is in place and the registered address of the club changes the club must give notice to the local licensing authority of the change and provide the certificate with the notice.
A club may apply to a local licensing authority to vary a certificate. The certificate should accompany the application. The local licensing authority may inspect the premises before an application is considered.
Fees may be payable for any type of application relating to a club premises certificate.
Will Tacit Consent apply?
Yes. This means that you will be able to act as though your application is granted if you have not heard from the local authority by the end of the target completion period of 56 calendar days (for new or variation applications).
Can I make my application online?
You can make your application online by going to the links on this page.
What can I do if my application fails?
Please contact your local authority in the first instance. A failed applicant will receive notice of the refusal of an application for a certificate or variation of a certificate from the local licensing authority.
If an application is rejected, the applicant may appeal the decision. Appeals must be made to the local Magistrates' court within 21 days of the decision appealed.
What can I do if I am unhappy about the licence conditions?
Please contact your local authority in the first instance. If a local licensing authority refuses an application for a variation the licence holder may appeal the decision. A licence holder can appeal against a decision to put conditions on a certificate or to exclude any club activity. Appeals may also be made against the variation of any condition.
Appeals against the decision of a review can be made.
A club may appeal against the withdrawing of a certificate. Appeals must be made to the local Magistrates' Court within 21 days of the decision appealed.
How can I make a complaint?
We would always advise that in the event of a complaint the first contact is made with the trader by you - preferably in the form of a letter (with proof of delivery). If that has not worked, if you are located in the UK, Consumer Direct will give you advice (see link on this page). From outside the UK contact the UK European Consumer Centre (see link on this page).
A club member may request a review of the certificate. The local licensing authority will give reasons for their response to the application in a notice.
Appeals must be made to the local Magistrates' court within 21 days of the decision appealed.
Are there other types of redress?
Any person living or involved in a business in the Borough that might be affected by the Club Premises may make representations to the local licensing authority before the certificate is granted or before amendments to a certificate are granted. If representations are made a hearing will be held to consider the application and the representations. Notices will be made by the local licensing authority detailing the reasons for any outcome. Interested parties who made representations will receive notice of a failed application.
Any person living or involved in a business in the Borough that might be affected by the Club Premises may request a review of the club premises certificate. The local licensing authority will give reasons for their response to the application in a notice.
Any person living or involved in a business in the Borough that might be affected by the Club Premises may appeal if they argue that a certificate should not have been granted or that different or additional conditions or limitations on activities should have been made. They may also appeal against any variation of a condition. Appeals against the decision of a review can be made. Appeals must be made to the local Magistrates' court within 21 days of the decision appealed.
Are there any trade association?
Working Men's Club and Institute Union (CIU)
Guidance - Club Premises Certificates
DOC, 164KB
A summary of the regulation relating to this licence.
www.legislation.gov.uk/uksi/2005/42/contents/made
Apply for a new club premises certificate
www.businesslink.gov.uk/bdotg/action/piplink?agency_id=340&service_id=3500010001
Tell us about a minor change to your existing premises or club
Tell us about a change to your existing details or club rules
Tell us about a change to your existing club premises certificate
Make an annual payment for an existing club premises certificate
Submit a club premises certificate declaration
Consumer Direct
www.direct.gov.uk/en/Governmentcitizensandrights/Consumerrights/index.htm
UK European Consumer Centre
www.ukecc.net/
Working Man's Club and Institute Union (CIU)
www.wmciu.org.uk/

redpajama_set_name: RedPajamaCommonCrawl


1 SHP = 3730.81 EAC at the rate on 2019-04-23 .
The page provides data about today's value of one pound in EarthCoins. The interactive form of the currency calculator ensures navigation in the actual quotations of world currencies according to "Open Exchange Rates" and displays the information in a graph.
The online converter will clarify the ratio between different currencies. For example, you can instantly convert 1 SHP to EAC based on the rate offered by "Open Exchange Rates" to decide whether you better proceed to exchange or postpone currency conversion until better times.
The value of 1 SHP in EarthCoins for the week (7 days) decreased by: -10.24 EAC (ten earthCoins).
The value of 1 SHP in EarthCoins for the month (30 days) decreased by: -56.58 EAC (fifty-six earthCoins).
The value of 1 SHP in EarthCoins for the year (365 days) decreased by: -266.41 EAC (two hundred sixty-six earthCoins).


text:
Israel's Netanyahu condemns protests against him, criticises media
Jeffrey Heller
August 2, 2020, 11:49 a.m. ·2 min read
Israelis protest against PM Netanyahu's alleged corruption and the way of handling the COVID-19 crisis in Jerusalem
By Jeffrey Heller
JERUSALEM (Reuters) - Prime Minister Benjamin Netanyahu struck back on Sunday at demonstrations calling for his resignation, accusing protesters of trampling democracy and the Israeli media of encouraging them.
Netanyahu, who was sworn in for a fifth term in May after an election, has often complained of press bias against him, and some of the charges he faces in a corruption trial relate to alleged attempts to seek favourable coverage from media barons in return for state favours.
Thousands of Israelis have been taking to the streets, including outside Netanyahu's Jerusalem home, to protest against alleged corruption and economic hardship stemming from lockdowns during the coronavirus crisis.
Netanyahu, who heads the right-wing Likud party, has denied wrongdoing in the three graft cases against him.
Criticising the protests and media at the weekly cabinet meeting, Netanyahu said that while demonstrators portray their campaign as an attempt to "preserve Israeli democracy, I see it as an attempt to trample democracy".
"These demonstrations are fuelled by a media mobilisation, the likes of which I can't remember," he said, accusing the Israeli press of "North Korean-like" uniformity in its alleged bias against him.
"They do not report the demonstrations - they participate in them. They add fuel," said Netanyahu, who returned as prime minister in 2009 after a first term from 1996-99.
Netanyahu, 70, said no one was trying to restrict the demonstrations, in which many of the protesters are young Israelis. Opinion polls have shown his popularity in decline.
Netanyahu's main coalition partner, Defence Minister Benny Gantz of the centrist Blue and White party, defended the demonstrations.
"The right to protest is the lifeblood of democracy," Gantz said at the cabinet meeting.
Legislator Tamar Zandberg of the opposition left-wing Meretz party said in a statement that Netanyahu was "marching in the footsteps of dark regimes".
(Editing by Timothy Heritage)
Amazon faces backlash from Indian ruling party lawmakers over web series 'Tandav'
A local official from India's ruling Hindu nationalist party on Sunday registered a police complaint against an Amazon Prime web series alleging it insults Hindu gods and goddesses, and threatened to launch a protest at the company's office in Mumbai. Protests against Amazon.com have been organised for Monday to warn it not to show scenes insulting Hindu gods and goddesses, Ram Kadam, a BJP member of the Maharashtra legislative assembly, said in a tweet after filing a complaint with police in Mumbai on Sunday. The political drama "Tandav" also drew the ire of other lawmakers from the Bharatiya Janata Party (BJP), causing fresh controversy for the e-commerce giant which last year had to withdraw dozens of rugs and doormats depicting Hindu gods from its international Amazon.com platform after a backlash in India.


Sitting here watching my girls pour frosted flakes on the floor...thinking about many things. My girls, the world, the universe, the frosted flakes on the floor, my dog, Vitamin C.
When this odor of Lavender comes to me. Trying to sniff it out. I have a super human sense of smell...always have..;) So here is this Lavender plaguing me. Cannot find a source for where it may be coming from?


Cindy has 35 years of experience in sewing and has provided custom sewing and embroidery services since 2003. Cindy began sewing out of necessity and it turned into a love of the creative process that transforms fabric into unique garments and home decor. I can help you with your embroidery or heat press jobs on shirts, coats, hats and anything fabric! From custom slip covers to repairing broken zippers, to embroidering logo's, Cindy's provides prompt personalized and friendly service.


An innovative concept for microwavable packaging has been realised by Ardagh, working in cooperation with designers at DéDutch and the University of Twente.
The new product is a bowl designed for at-home fondue and is being rolled out by dairy brand Emmi in supermarkets Canada, the US, and the Netherlands.
Cheese in the All In One Fondü metal bowl is melted and then held off the eating surface in a black plastic cradle.
Marcel Zbinden, Emmi's head of speciality cheese, explains: 'Convenience and quick preparation have become a more and more important trend. This concept has it all and it will delight fondue lovers worldwide.


The following calculation-method is to be considered only as a guideline, since many unpredictable factors may require changes.
V = Periferal Speed in m/min.
500 when the bearing is 100% dry.
1000 when the bearing is greased at fitting.
2000 when the bearing is greased regularly.
5000 when the bearing is greased automatically or submerged in the lubricant.
This rule is valid for V > 25 m/min. If V < 25 m/min., a higher Surface Pressure P is permitted.
Surface Pressure P max. = 550, when V = 0, at +20C.
At 500 revolutions/min.: V = 10 x p x 500 = 15.700 mm/min. = 15,7 m/min.
When the NYLONIT bearing is pressed into a countersunk hole with H7 tolerance it provides a bearing clearing for a shaft with h7 tolerance of 0,5 – 1,0% of the shaft-diameter. If a smaller bearing-clearance is required, i.e. at low loads and rotation-speed, this is achieved by pressing the bearing-bushing into a corresponding smaller hole.
Please note: The tolerance is in the bearing-clearance (wall-thickness). Our dimensions are stated respectively for shaft-diameter and bearing-house-diameter and can therefore not be used as control-dimensions before the bearing has been fitted.
BEAR IN MIND: ONE DROP OF OIL WHEN FITTING MEANS LONGER LIFETIME AND LOWER FRICTION !


text:
Showing results for tags 'fictional country'.
fictional country
Dannian Superliga (Kabana SC up!) (C&C wanted)
NoE38_Concepts posted a topic in Concepts
I have already attempted this twice, but I was just new to designing then and wasn't ready for a project like this. Now I feel like I can do it, and hope to improve my logo-making skills along the way. Now, onto my country, Dannia, which is an island Northwest of New Zealand. It is around 341,000 km2 (Approximately the size of Finland) and has a population of 16.6 million people. The capital city is Kabana, with a population of 1.9 million. (Not all cities will have a team) The league logo is a large letter D with a eight-sided star, the national symbol, acting as the hole in the centre. Inside of the star is a stylized soccer ball/futbol, telling people what sport the league is. The logo is in red, black, and white, the national colours. First team should be up soon!
fictional soccer league
dannia
Fictional Soccer League Take 2
This is take 2 for my fictional soccer league. My country is called Dannia, has a population of 18 million, and is around the size of Finland. The League's 10 teams will be based in 5 main cities, with Kabana, the capital, being the home of 6 clubs. League Logo: (this means 'super league'' in Dannian) The first team will be up soon!
Fictional Country: Dannian Premier League
It seems like a lot of people have fictional countries these days, so I guess I should post mine. A while ago, I made a country called Dannia. The capital city is Kabana. Map: Along with it, I made the Dannian Premier League. This league has 9 teams. Because I'm using paint, the graphics will be bad, so sorry about that. The first team, the Kandres Waves FC, is coming soon!
Offical Gutland Athletcis Homepage (HAH)
sleuthpanther posted a topic in Concepts
Hey guys so I just made this extremely long, funny (er) post about this but of course the damn thing crashed and its gone. So heres to starting over. So Gutland is a fictitious country I made up what must of been years ago, and now I found it and i'm rebooting it and "my very own hopefully less corrupt NCAA". What I hope to do is release at least 30 media guides for the 30 D1 schools in Gutland stuffed with branding, logos and uniforms and facts for football and mens baseball and basketball. Those are the three I have most fun doing, so that's what I'm sticking with. On top of that I plan on a much smaller d2, and some extra tidbits here and there. I'm doing this now because I'm on break, once I'm back in school posting will be more spontaneous. I'm using a strange combination of Gimp and paint.net but it gets the job done. Well, without much further ado heres Gutland! Ok much briefer history than my last post. Gutland is slightly north of Virginia in the Atlantic Ocean. It was discovered by Scandanavians and named Gutland. Next French colonized the South and English colonized the North and Central. Irish snuck into some gaps between the two. For a while it was peaceful between the two with the English fighting many wars with the Tonka and Creek native American tribes to the North. Eventually france and England fought, France's military was dispelled but much of French culture in the south remained. Germans later colonized swaths of Land to Gutland's eastern shores. Gutland aided the US in many wars from the world wars to Vietnam, and for this the US allowed Gutland to remain independent. Now here are some maaaaaps. Again I had much longer descriptions of the capitols but now I'm a little bugged, so heres some little ol descriptions. Tonka City- Farming city, large metro, large pop., rural outside of metro, coastal, largest national park, forest/flat terrain Stackhouse- Shipping/freight city, large coastal influence, highest density in country, average quality of life very low Silversmith- largest producer of steel/iron, second highest altitude, rural scattered metro, heavily forested Allentown- next to largest river in country, largest factories, largest producer of freight, surprisingly high standard of life Saint Williams- highest average income, lowest average altitude, large wealthy metro, prides itself on high conviction rates Fort Pierre- most sought after art/architecture in country, depends on tourism, heavy costal influence Sablewood- large trading hub in South, largest producer of boat/airplane parts, big lumber/fishing producer Trafalgar- Capitol of Trafalgar, City and state(like NYC) highest population in country Thanks for stopping by guys, I have one primary logo left so I should have a logo map done soon to give you guys a sneak peak, if you have any other questions about the project OR the country it'self I'd be very happy to answer. Hope you all enjoy and have a great night (day?).
Fictional Soccer League: Monarch Premier League - Nenor City (2/20)
Welcome to the Monarch Island Premier League! The league is home to 20 teams from 2 countries. Monarch Island is south-west of Ireland and West of France in the Atlantic Ocean. It's countries include: The Provinces of Taurun- primarily English and has a strong resemblance to the USA in things like suburbs and cities, but many are from Ireland and the UK. Republique de Larcons- Salut! Bienvenue to Larcons! Larcons again, like Taurun has American-style suburbs and cities but is almost exactly like France in every other way. The league (2015/16) consists of: Bolian FC Nenor Bay Nenor City FC Carn Orvill FC AFC Winchester Northan United Pioneer Tallon Jefferson North Bay Tomas Island City Cavalry (Larcons Ville) AFLV (Association Football Larvcons Ville) Cape Laval Reims Isle FC Le Port Le Mans AC Montpellier Saint-Paul Wellington SC Malar Last Year Champions (14/15) Nenor City Newly Promoted Northan United Wellington Reims Isle FC Leagues in the Federation Premier League Division 2 Division 3 Lower Tiers You may recognize this country from 9jakepenny. This is because he is actually my cousin who has given up on the country and he has given my permission to explore the island and develop the league. He may make some notes here and there. Bolian FC Bolian FC has been one of the most famous teams in the league's history. They were established in 1934 and have lifted the league trophy 11 times. They were the first team to repeat championships (2005/06--2006/070 in over 22 years. Recently the club has been doing great as they lifted the cup in 2014/15.
fictional league
monarch premier league


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KDnuggets Home » News » 2016 » Sep » Tutorials, Overviews » 9 Key Deep Learning Papers, Explained ( 16:n34 )
9 Key Deep Learning Papers, Explained
http likes 842
Tags: Academics, Deep Learning, Explained, Neural Networks
If you are interested in understanding the current state of deep learning, this post outlines and thoroughly summarizes 9 of the most influential contemporary papers in the field.
By Adit Deshpande, UCLA.
In this post, we'll go into summarizing a lot of the new and important developments in the field of computer vision and convolutional neural networks. We'll look at some of the most important papers that have been published over the last 5 years and discuss why they're so important. The first half of the list (AlexNet to ResNet) deals with advancements in general network architecture, while the second half is just a collection of interesting papers in other subareas.
1. AlexNet (2012)
The one that started it all (Though some may say that Yann LeCun's paper in 1998 was the real pioneering publication). This paper, titled "ImageNet Classification with Deep Convolutional Networks", has been cited a total of 6,184 times and is widely regarded as one of the most influential publications in the field. Alex Krizhevsky, Ilya Sutskever, and Geoffrey Hinton created a "large, deep convolutional neural network" that was used to win the 2012 ILSVRC (ImageNet Large-Scale Visual Recognition Challenge). For those that aren't familiar, this competition can be thought of as the annual Olympics of computer vision, where teams from across the world compete to see who has the best computer vision model for tasks such as classification, localization, detection, and more. 2012 marked the first year where a CNN was used to achieve a top 5 test error rate of 15.4% (Top 5 error is the rate at which, given an image, the model does not output the correct label with its top 5 predictions). The next best entry achieved an error of 26.2%, which was an astounding improvement that pretty much shocked the computer vision community. Safe to say, CNNs became household names in the competition from then on out.
In the paper, the group discussed the architecture of the network (which was called AlexNet). They used a relatively simple layout, compared to modern architectures. The network was made up of 5 conv layers, max-pooling layers, dropout layers, and 3 fully connected layers. The network they designed was used for classification with 1000 possible categories.
Trained the network on ImageNet data, which contained over 15 million annotated images from a total of over 22,000 categories.
Used ReLU for the nonlinearity functions (Found to decrease training time as ReLUs are several times faster than the conventional tanh function).
Used data augmentation techniques that consisted of image translations, horizontal reflections, and patch extractions.
Implemented dropout layers in order to combat the problem of overfitting to the training data.
Trained the model using batch stochastic gradient descent, with specific values for momentum and weight decay.
Trained on two GTX 580 GPUs for five to six days.
Why It's Important
The neural network developed by Krizhevsky, Sutskever, and Hinton in 2012 was the coming out party for CNNs in the computer vision community. This was the first time a model performed so well on a historically difficult ImageNet dataset. Utilizing techniques that are still used today, such as data augmentation and dropout, this paper really illustrated the benefits of CNNs and backed them up with record breaking performance in the competition.
2. ZF Net (2013)
With AlexNet stealing the show in 2012, there was a large increase in the number of CNN models submitted to ILSVRC 2013. The winner of the competition that year was a network built by Matthew Zeiler and Rob Fergus from NYU. Named ZF Net, this model achieved an 11.2% error rate. This architecture was more of a fine tuning to the previous AlexNet structure, but still developed some very keys ideas about improving performance. Another reason this was such a great paper is that the authors spent a good amount of time explaining a lot of the intuition behind ConvNets and showing how to visualize the filters and weights correctly.
In this paper titled "Visualizing and Understanding Convolutional Neural Networks", Zeiler and Fergus begin by discussing the idea that this renewed interest in CNNs is due to the accessibility of large training sets and increased computational power with the usage of GPUs. They also talk about the limited knowledge that researchers had on inner mechanisms of these models, saying that without this insight, the "development of better models is reduced to trial and error". While we do currently have a better understanding than 3 years ago, this still remains an issue for a lot of researchers! The main contributions of this paper are details of a slightly modified AlexNet model and a very interesting way of visualizing feature maps.
Very similar architecture to AlexNet, except for a few minor modifications.
AlexNet trained on 15 million images, while ZF Net trained on only 1.3 million images.
Instead of using 11x11 sized filters in the first layer (which is what AlexNet implemented), ZF Net used filters of size 7x7 and a decreased stride value. The reasoning behind this modification is that a smaller filter size in the first conv layer helps retain a lot of original pixel information in the input volume. A filtering of size 11x11 proved to be skipping a lot of relevant information, especially as this is the first conv layer.
As the network grows, we also see a rise in the number of filters used.
Used ReLUs for their activation functions, cross-entropy loss for the error function, and trained using batch stochastic gradient descent.
Trained on a GTX 580 GPU for twelve days.
Developed a visualization technique named Deconvolutional Network, which helps to examine different feature activations and their relation to the input space. Called "deconvnet" because it maps features to pixels (the opposite of what a convolutional layer does).
DeConvNet
The basic idea behind how this works is that at every layer of the trained CNN, you attach a "deconvnet" which has a path back to the image pixels. An input image is fed into the CNN and activations are computed at each level. This is the forward pass. Now, let's say we want to examine the activations of a certain feature in the 4th conv layer. We would store the activations of this one feature map, but set all of the other activations in the layer to 0, and then pass this feature map as the input into the deconvnet. This deconvnet has the same filters as the original CNN. This input then goes through a series of unpool (reverse maxpooling), rectify, and filter operations for each preceding layer until the input space is reached.
The reasoning behind this whole process is that we want to examine what type of structures excite a given feature map. Let's look at the visualizations of the first and second layers.
Like we discussed in Part 1, the first layer of your ConvNet is always a low level feature detector that will detect simple edges or colors in this particular case. We can see that with the second layer, we have more circular features that are being detected. Let's look at layers 3, 4, and 5.
These layers show a lot more of the higher level features such as dogs' faces or flowers. One thing to note is that as you may remember, after the first conv layer, we normally have a pooling layer that downsamples the image (for example, turns a 32x32x3 volume into a 16x16x3 volume). The effect this has is that the 2nd layer has a broader scope of what it can see in the original image. For more info on deconvnet or the paper in general, check out Zeiler himself presenting on the topic.
ZF Net was not only the winner of the competition in 2013, but also provided great intuition as to the workings on CNNs and illustrated more ways to improve performance. The visualization approach described helps not only to explain the inner workings of CNNs, but also provides insight for improvements to network architectures. The fascinating deconv visualization approach and occlusion experiments make this one of my personal favorite papers.
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There have been any number of fundraising announcements in the past two weeks. And as compelling as that news is, it's even more exciting to see the companies putting that money to work. Like Rigado, for instance. Which recently raised $15 million. And that led to a bunch of open jobs. Like nine of them.
Every once in a while, you get to be present to witness the establishment of a widespread platform. A platform that provides the means of making a market. Sometimes, it's the first to market—like the iPhone or Roku. Sometimes, it's a fast follower—like Microsoft Explorer or Google. We've seen it happen time and time again. With the Web and Mobile and Streaming Media. But it's rare to see that happen locally.


The Lenbachhaus is playing host to a new exhibition starting Tuesday. I'm a Believer is all about pop art and contemporary art – from Warhol to Austrian painter Maria Lassnig, Daniel Man to Sigmar Polke. The vernissage is on Monday, from 7pm onwards.
On Tuesday, Austrian band Wanda will play a sold-out show in Zenith. They released their last album Niente last year, and are still riding on the waves of success from their 2015 hit single Bologna (still a firm favourite in my household).
The excellent Nathaniel Rateliff and The Night Sweats are playing a sold-out show in the Muffathalle on Wednesday.
On Saturday, Wallis Bird is playing a Hauskonzerte gig in MMA. Starkly contrasting her gig, LA rockers Black Label Society are playing Backstage Saturday. They've been going for twenty years, and released their tenth studio album, Grimmest Hits, in January of this year.
Jamie Lawson rounds off the week, with a show at Technikum. The singer-songwriter was the first musician to be signed to Ed Sheeran's label, Gingerbread Man Records, and he's most famous for his catchy single Wasn't Expecting That.
And finally, all the excellent Oscar movies are in cinemas here. I, Tonya is showing in Cinema (in English) on Thursday, at 7pm (it's also showing in English in Atelier 2 on Monday). Call Me By Your Name is showing in OV next Wednesday at Neues Maxim in Neuhausen as well as all week in City Kino 2, and Three Billboards is showing in City Kino 1 on Monday and Tuesday next week. Monopol will also screen Oscar winner Shape of Water throughout next week in English.
I'm also excited that the Monopol is showing the Jane Goodall documentary on Monday next week (5pm) – in English, with German subtitles.


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A coalition of student protesters presented the Yale Investments Office with an open letter on Oct. 26 demanding that the University withdraw Yale-owned real estate from a deal allowing the construction of a transmission line through New Hampshire.
The proposed transmission line, called Northern Pass, would carry energy from Canada's hydropower plants through New Hampshire and into New England. While a portion of the 192-mile transmission line would be underground, some forest areas would have to be cleared for construction. Protesters cited environmental and social justice concerns as their reasons for opposing the project.
Through an investment partner, Yale owns a 24-mile piece of land integral to the development of the Northern Pass under its current specifications, said Jerry Curran, chair of the New Hampshire chapter of the Sierra Club. Without that land, the project would face serious setbacks, he added.
Much of the criticism focuses on the role of Canadian hydropower company Hydro-Quebec in the project. Hydropower, unlike wind and solar energy, has severe climate costs, including higher greenhouse gas emissions and a high carbon footprint, according to Curran.
Hydro-Quebec spokeswoman Lynn St-Laurent disputed those claims about hydropower, arguing that it is "absolutely false" to say that Hydro-Quebec reservoirs produce larger carbon footprints than other sources of renewable energy.
Yale's investment manager Bayroot LLC originally leased the land in question to the energy company Eversource in 2012. Last summer, Eversource exercised an option to renew that lease until 2110. Over the following months, student groups, concerned New Hampshire residents and other affected parties unsuccessfully lobbied the University to pull out of the deal, Colon said.
Yale responded to complaints in a June 20 press release explaining that the University had little involvement in organizing and upholding the lease. According to the release, most of the Yale endowment is managed by external managers, who are given discretion to invest in projects without first consulting the University. Wagner Forest Management, a company hired to manage the land, leased the 24 miles of contested timberland to Eversource for this project. The Investments Office declined to comment on the open letter.
While the Northern Pass is still under review by the New Hampshire Site Evaluation Committee, Eversource spokesman Martin Murray said the company is confident that the project will reduce New England's reliance on less sustainable, more expensive fossil fuels. In doing so, carbon emissions will go down by three million tons each year, saving the region $600 million annually, Murray said.
"There is a real serious objective to diversify the sources of energy in New England, to find clean sources of energy and sources that will lessen costs," Murray said.
In addition to their qualms about the environmental impact of the line, protesters focused their ire on Hydro-Quebec's strained relationship with the Pessamit First Nation in Canada, an Innu community that has lived for centuries in the region, which now houses several hydropower dams.
In a letter sent to the Yale Investments Office in May, Pessamit Innu First Nation Chief René Simon claimed that Hydro-Quebec, Eversource's Canadian partner, has operated illegally on Pessamit land and caused severe damage to fisheries and natural ecosystems.
In that letter, the Pessamit people invited a delegation from the Yale Investments Office to come to Canada to witness the severity of hydropower's impact on the natural environment.
"When Yale allows this injustice to be committed against the Pessamit people, they send the message that they don't care about the oppression of marginalized people everywhere," Colon said.
Yale has not responded to any of the Pessamit people's attempts to open communication, she added.
In response, St-Laurent said Hydro-Quebec has not violated any historical treaties concerning the Pessamit Innu. The company always develops projects and operates in accordance with the legal framework and aboriginal rights, she added.
While he said Eversource is aware of the criticism of the project, Murray suggested that some of the opposition may result in part from negative advertisements potentially funded by other corporate stakeholders.
The graduate student union Local 33, the Yale Student Environmental Coalition and the Association of Native Americans at Yale were among the groups that backed the open letter.
Correction, Nov 7: A previous version of this article mistook the New Hampshire Site Evaluation Committee with the United States Securities and Exchange Commission.


text:
Q: Mutated vowels (in german: "Umlaute") in Aptana 3 terminal I use Aptana Studio 3 for rails development together with git versioning. In my commit messages I'd like to use mutated vowels (Umlaute). In Terminal (Mac OSX) everything works fine, but in the Aptana terminal I get strange characters (btw: in the Aptana editors mutated vowels work). Is there a way to get this working?
Thanks for your help!

A: This has been fixed in Aptana Studio 3.0.2 release.

redpajama_set_name: RedPajamaStackExchange


text:
Connect with Babbage Cofounder
Lexington | Frankfort | Louisville
Northern KY | Cincinnati | Washington D.C.
Frankfort Office
KYGA18 day 43 begins today!
We are 2/3 of the way through the session. For the first time in almost a century, a series of budget-related bills from a Republican-led House has been proposed and passed out of the House. Representative Steven Rudy (R-Paducah) introduced a series of bills this week, all of which were heard in committee: HB200– the complete two-year budget, HB202– road projects, HB203– judicial branch, HB204– legislative branch, and HB366– revenue. This is also the earliest a budget has been passed out of the House, in the past budgets have been introduced in the final days.
"The moving sidewalk is ending." – Jack Fox
Jack Fox, a Louisville voice-over professional who issues this familiar recorded warning in numerous airports around the country had a voice role in Oscar winner The Shape of Water. Michael Shannon, a native of Lexington, was also cast in the film and is a two-time Academy Award nominee. #KentuckyProud
Article: 'Vice President Mike Pence to visit Versailles Wednesday'
Article: 'Some of the 70 programs cut in Gov. Bevin's budget spared by House; some not.'
Week in Review February 26 – March 2
Wednesday was a big day at the Capitol. First was the pension discussion (SB1). Hundreds of teachers flocked to the Annex to listen and show their opposition to the proposal. Later in the afternoon was the Budget discussion. Here are the major items put forth:
$0.50 per pack cigarettes tax increase
$0.25 per opioid pill on tax on prescriptions
6% reduction in most state agencies
Increase in pension funding
Increase in K-12 education
Increase in student transportation
Added 14 programs back to the 70 programs that were cut in the Governor's proposal.
The cigarette and opioid tax would add $375 million in state revenue over the next two-years. The House restored funding to higher education. For example, University of Kentucky had $16 million added back.
SB95 Medically Necessary Fertility Preservation called "Melissa's Law" enables children and young adults who battle cancer to preserve options for a biological family after chemotherapy and radiation treatments. With the leadership of sponsor Senator Kerr (R-Fayette) and a host of other cosponsors, SB95 passed unanimously and heads to a Senate floor vote possibly today. You can watch parts of the moving testimony on the KET legislative update (scroll to 8:05-11:55).
School safety is of utmost importance with the recent, tragic shooting in Marshall County and then in Parkland, FL. On Thursday, a joint education meeting focused on this topic and featured a national school safety spokesman who shared testimony based on years of experience. A wide array of bills have been proposed, some of which are listed below:
SR172 Teachers and Firearms: This resolution reaffirms urges the board of education or board of trustees of a school to allow teachers and other school personnel to carry firearms for their own protection. This was passed out of committee 8-3.
HB554 School Safety: Representative Gooch (R-Providence) filed a bill to require that at each school without a school resource or security officer, the local board shall implement an emergency response team.
HB602 Prohibit Bumpstocks: This legislation, filed by Representative Coursey (D-Symsonia) of Marshall County, aimed at eliminating the sale or transfer of bump stock devices, trigger cranks, and other items designed to accelerate the rate of fire without turning a firearm into a fully automatic firearm; create penalties; provide for the destruction of the items after a conviction and any appeals.
HB604 Trauma Informed Schools: In response to the fatal school shooting at his alma mater, Rep. Coursey also filed this bill that requires each school to employ at least one mental health professional for every 1,500 students; require the department of education or make available a toolkit to assist school districts in developing a trauma-informed approach in their schools. That would also require each local board of education to develop a plan for implementing a trauma-informed approach in its schools by the 2020-2021 school year.
Here's a look at what's coming up
March 7 Northern Kentucky Day in Frankfort. Our firm is a cosponsor for this event.
March 5 is the start of 14 working days for House and Senate until March 22
March 27-28 Concurrence only days — House and Senate finish regular business
March 29 Veto period begins
April 6 Opening day of Spring Meet at the historic, iconic Keeneland Race Course
April 9 Veto period concludes
April 12-13 Complete all action, Days 58 and 59 of Session
April 15 SINE DIE
The Session Calendar and the Committee Schedule are great to bookmark. We'll monitor Committees for you as bills pertaining to your issues come through.
Our team will continue to send weekly reports to share top stories and any information that may be helpful. See our Facebook and Twitter pages for real-time updates.
Kentucky Legislative Weekly Wrapup video.
March 6, 2018 Latest News
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Happy Monday, friends. I think the fabric choice for today's outfit matches what's going on in my life. You know what they say - Into each life a little rain must fall. So, what's going on you may ask? Well, yesterday, I was all geared up to run the North Face Endurance Series 10k on what is rated their most technical trail run. I ran this race 2 years ago and it certainly was a doozy. I am not a trail runner by any means. AND I went into it saying I was going to take it slow because I didn't want to mess up an ankle or a knee this close to the half marathon I have been training for. Well, my ankles and knees are (mostly) okay. We started the race and about a quarter of a mile in, I tripped on a downhill and I knew once I hit the ground and saw white I was in trouble. I got back up and tried to keep going. I couldn't. I couldn't move my arm. I walked back to the start line to the med tent where I was in so much pain I was in tears and nearly passed out/threw up. So, I got to take my first ride in an ambulance. They initially thought I dislocated my shoulder, but it turns out I fractured my scapula (shoulder blade). So, now Im unable to use my left arm. I'm in horrible pain. I'm basically useless. I have an appointment tomorrow with an orthopedist.There is some thought I may have torn a ligament but won't find that out until after an MRI.
The good news is I have 2 outfits done for this week. The scary thing is I have two other days to sew for. I am so dedicated to this challenge, I have to figure out someway to do it. I don't want to stop now. It's bad enough that my running season is over.
So, Im in a funk right now. I hate being dependent on people and I hate not being able to get done what I need to get done. Hopefully, I won't have to have surgery.
So, tonight I bring to you the upcoming release from Heidi and Finn that I had the privilege to pattern test. You can find Heidi and Finn patterns on Etsy at https://www.etsy.com/shop/heidiandfinn?ref=l2-shop-info-name and on Facebook at https://www.facebook.com/groups/602746356411507/. This pattern is scheduled to be released Wednesday and they have lots of other great patterns.
And what do you think of our new look?? I love it. It was done by Jenny at FrenchPressMornings on Etsy!
Pray for me so we can keep these outfits coming!!


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

Massive stars shape the Galaxy via radiative and mechanical feedback and appear as lighthouses of star formation. The feedback is primarily visible through optical emission of ionized (\hii) regions in the plane of the Galaxy \citep[e.~g. recent H-alpha surveys by][]{SHASSA, IPHAS}. Theory predicts that shock waves, related to expansion of the \hii{} regions, compress the neutral gas and dust and collect it into moving dense molecular layers, \citep[e.g.][]{Spitzer_1978}. One of the most studied dense shocked layers on the border of an \hii{} region is the Orion Bar photo-dissociation region (PDR, the region between ionization front and attenuated cold molecular gas), which has already been observed with high angular resolution in optical, infrared and millimetre wavelengths \citep[e.~g.][]{McLeod_2016, Goicoechea_2016, Berne_2022}. A steady-state structure of the Orion Bar PDR where dissociation fronts of different molecules are separated from each other by several values of $A_{\rm V}$ was developed by \citet{Tielens_1985,Tielens_1993}. Only after the appearance of the first ALMA data towards the PDR, dynamical effects have been revealed by \citet{Goicoechea_2016} and confirmed numerically by \citet{Kirsanova_2019b}. Since the Orion Bar PDR is a unique object due to its proximity, many other PDRs are all less studied. Moreover, retirement of the SOFIA telescope, which brought a bulk of important observational data towards PDRs, leads to difficulties in getting more data about PDRs. Therefore, our knowledge about PDRs are highly limited by the strong selection effect and every new study of their properties is important.

The southern \hii{} region RCW~120 is powered by an O6-8V/III ionizing star \citep{Martins_2010} and has a radius of 250\arcsec. Simple ring-like geometry of RCW~120, which resembles a projection of a 3D spherical shell, makes it attractive to study. However, the position of the ionizing star does not corresponds to the center of the neutral envelope of the \hii{} region, see Fig.~\ref{fig:obsregion}. Moreover, the maximum of the free-free continuum emission is shifted to the south up to 1.5\arcmin{} in the plane of the sky. Therefore, the simple geometry of RCW~120 might be illusory. RCW\,120 is one of the nearest \hii\ regions to the Sun, 1.34~kpc distant~\citep[][]{Russeil_2003}\footnote{We prefer not using 1.7~kpc from \citet{2019ApJ...870...32K} because GAIA gives the best distances for unobscured stars but the extinction $A_{\rm V} = 4.4$ towards RCW~120, see \citet{Zavagno_2007}. }. Physical radius of the \hii{} region is therefore about 1.6~pc but the mean projected distance between the ionizing star and the southern neutral border of the \hii{} region is about 1~pc. The cold neutral material around RCW\,120 consists of several condensations arranged to the shell-like structure, the condensations contain embedded young stellar objects (YSOs) \citep{Zavagno_2007,Deharveng_2009}. The most massive is a Class~0 YSO with $M_{\rm star}=8-10 M_{\odot}$ (source\,2 in ~\citet{Figueira_2017}, S2 below). Recently, \citet{Luisi_2021} found an expanding continuous shell around RCW\,120 due to a stellar wind impact, observing the \cii{} emission at 158~\micron.

The neutral environment of RCW~120 has different geometry compared with the view at the \cii{} line. The PDR appeared in flattened face-on molecular cloud partly embedded into a low-density envelope \citep[see][]{Anderson_2015, Kirsanova_2019, Kabanovic_2022}. Therefore, RCW~120 is not a simple 3D sphere or 2D ring, but different parts of the object can be modelled by a 1D or 2D numerical model or by their combination. Modelling of the region as a whole can probably be done in some approximation such as a smoothed-particle hydrodynamics approach \citep[see][]{2015MNRAS.452.2794W}.

Since RCW~120 is expanding, one can expect to find the dense shocked layer in its PDR. While the mentioned above authors studied RCW~120 with spectral lines of CO and its isotopologues, none of these studies had sufficient spatial resolution to resolve the shocked layer. \citet{Kirsanova_2019} calculated the physical structure of the RCW~120 PDR and found a width of the dense moving layer of 0.1~pc. Using single-dish ground-based telescopes, this layer can be resolved only with the APEX telescope and \co{} lines at a frequency $\approx 660$~GHz \citep[Fig.~1 in][]{2018abmc.conf..284K} or by ALMA. In this study, we present the resolved observations of the dense shocked layer in RCW~120.

 \begin{figure}
\includegraphics[width=\columnwidth]{fig1.pdf}
\caption{Image of RCW\,120 at 70\micron{}. Color scale shows emission of neutral material around the ionized gas. The position of the ionizing star of RCW~120 is marked as a red star. The 843~MHz radio continuum emission corresponding to free-free emission of the ionized gas is shown with white contours linearly spaced from from 0.1 to 0.4 Jy/beam. The 870\,$\rm \mu$m contours for 0.4, 2.0 and 10.0 Jy/beam are shown in black. Black circles show the locations of compact sources described by \citet{Figueira_2017} (their Table~5). The sizes of the circles depend linearly on the source masses \citep[$M_{\rm env}$ from][]{Figueira_2017} here and on the following figures. The area, observed in the \co{} line, is shown by the red rectangle.}
\label{fig:obsregion}
\end{figure}

\section{Observational data and numerical simulations}\label{sec:obs}

We performed new observations of the RCW~120 PDR and combined their results with simulations of the region in order to distinguish between large-scale phenomena, related to the kinematics of the \hii{} region, and local star-formation processes, related to star-forming activity, on molecular emission maps.

\subsection{\co{} and \tco{} observations}

The observations were carried out using the Atacama Pathfinder EXperiment telescope (APEX) in Chile on 15 and 17/18 of October 2019 and 10 July 2021, as projects O-0103.F-9301A-2020 and O-0107.F-9318A-2021 (PI: Kirsanova M.~S.) within the Swedish operated share. The receiver used was the Band~9 part of the SEPIA bundle \citep{Baryshev_2015,Belitsky_2018}, also called SEPIA~660. In case of $^{12}$CO (2019), it was tuned to 691~GHz (the line frequency is 691473.076~MHz) covering the sideband ranges 685-693~\&~701-709~GHz, and for $^{13}$CO (2021) it was tuned to 661067.276~MHz covering 655-663 \& 671-679~GHz. The spectral resolution in the FFT spectrometer used was about 61~kHz (26~m~s$^{-1}$) with 65536 channels per every 4~GHz. The data were calibrated to antenna temperature in real-time using the standard {\it apexOnlineCalibrator} package, but we later additionally applied factors of $\eta_{\rm mb} = 0.40$ and~0.53 for \co{} and \tco, respectively\footnote{https://www.apex-telescope.org/telescope/efficiency/index.php}, to arrive at the main beam temperature scale. The spatial resolution of the data was 9\arcsec, corresponded to 0.058~pc at the distance of RCW\,120.

We observed a region with different physical conditions: from the irradiated side of molecular clump on the border of the ionization front (photo dissociation region, RCW\,120~PDR below) to the outskirts of the clump, see Fig.~\ref{fig:obsregion}. The region contains several massive YSOs. For $^{12}$CO, the region was mapped using the OTF mapping mode to cover 175\arcsec{} by 90\arcsec{} rotated 45$^\circ$\ in the equatorial system (the long side extending from southeast to northwest, see Fig.~\ref{fig:obsregion}). The rows/columns in the map were alternatingly observed along the x- and y-directions with a data dump time of 1.0 seconds and a step of 3.1\arcsec. The off-position was chosen at the direction $\alpha=17\rm ^h$12$\rm ^m$08.000$\rm ^s$, $\delta=-38^\circ$36\arcmin03.00\arcsec (J2000). The weather was rather poor with $0.9<{\rm PWV}<1.6$~mm (corresponding to $T_{\rm sys} \approx 1000-4000$~K) for the $^{12}$CO map given this atmospheric window but relatively stable and calibrations were inserted more often to ensure consistent intensity calibration.

The $^{13}$CO observations were carried out as an 90\arcsec{} OTF strip cutting through the peak integrated intensity position of the $^{12}$CO map at a right angle to the long axis of the map. The data dump time and step size were the same as for the $^{12}$CO observations. Total observational time was 1.7~h. The weather conditions were better for the $^{13}$CO observations with $0.6<{\rm PWV}<0.7$~mm and typical $T_{\rm sys} = 730$~K.

The gridding of the data and the baseline correction were performed using the CLASS package from the GILDAS\footnote{http://www.iram.fr/IRAMFR/GILDAS} software. Further analysis was done with Astropy \citep{astropy:2013, astropy:2018}, and APLpy \citep[][]{aplpy2012, aplpy2019} was used for representation. Final fits-cubes were proceeded to the common grid with the step size of 3.1\arcsec{} in x- and y-directions. Typical noise level ($1\sigma$) of the regridded data is 1.5-1.7~K.

\subsection{Archival data}

We used the multi-wavelength data from various archives. In the section, we briefly describe them and provide needed references. The {\it Herschel} HIGAL data at 70~\micron{} \citep{2010PASP..122..314M} and the SUMSS 843~MHz radio continuum emission \citep[][]{Bock_1999} were used to outline general geometry of the neutral environment RCW~120 and the ionized gas, respectively. The ATLASGAL 870~\micron{} emission was used to locate dense and cold molecular clumps \citep{2009A&A...504..415S}. The [\cii] line emission at 158~\micron{} obtained as a part of the FEEDBACK Legacy Program \citep[][]{2020PASP..132j4301S} were downloaded from the {\it SOFIA} archive and used to study the irradiated side of the RCW~120 PDR together with the {\it Spitzer} data at 8~\micron{} \citep[][]{Zavagno_2007}.  We also used the $^{12}$CO and $^{13}$CO (3--2) data \citep{Kabanovic_2022} to study dependence of our conclusions on spatial resolution.

\subsection{Numerical simulations}

We simulated the physical and chemical structure of RCW~120 using the MARION model according to the approach by \citet{Kirsanova_2019}. In the present study, all the model parameters were taken the same as those authors did. We took the model results at the moment $5.8\times10^5$~yrs from the beginning of the \hii{} region expansion when the \hii{} region has the radius about 1~pc. We note that this model time should not be considered as an age of RCW~120, because geometry of the region is not spherical and density distribution is not uniform. However, our 1D model can be used to study the shocked region on a scale of a particular molecular clump because we are not pretending to simulate the line profiles, related to geometry, but interested only in the line brightness, related to the energy of the region. Using the simulated physical and chemical structure, we applied RADEX software~\citep[][]{vanderTak_2007} in order to model brightness of the various lines of CO, $^{13}$CO and \cii. Coefficients for collisions with H$_2$ were used for all considered emission lines because this molecule is the most abundant collision partner in our model. Using APEX beamwidth at 1.3, 0.9 and 0.4~mm (27\arcsec, 18\arcsec and 9\arcsec) as well as {\it SOFIA} beamwidth at 158~micron (15\arcsec), we simulate the brightness of molecular lines from RCW~120 for those telescopes.

\section{Results}\label{sec:res}

\subsection{Observed \co{} and \tco{} line emission}\label{sec:geom}

Spatial distributions of the \co{} peak and the integrated intensity are different as they are defined by large-scale and local phenomena, respectively. Namely, the peak intensity of the \co{} emission in Fig.~\ref{fig:obsemission} has a layer-like spatial distribution coinciding with the [\cii{}] emission in the RCW\,120 PDR. The peak \co{} intensity drops sharply on the irradiated side of the PDR but decreases smoothly on the attenuated side. The layer of the bright \co{} emission appears parallel to the ionization front (compare Fig.~\ref{fig:obsregion} and~\ref{fig:obsemission}) and does not become warped around the border of the dense and cold material, traced by ATLASGAL 870\,$\mu$m contours (compare left and right panels in Fig.~\ref{fig:obsemission}). Therefore, the bright CO-layer represents a shell of irradiated gas related to large-scale gas distribution created by RCW\,120.

The shortest projected distance from the ionizing star (shown in Fig.~\ref{fig:obsregion}) to the bright CO-layer is 146.5\arcsec, corresponding to \innersize. Physical width of the layer, in the direction perpendicular to the ionization front, is $\approx 0.10-0.15$~pc as we deduce from spatial distribution of the peak intensity in Fig.~\ref{fig:obsemission}. Note that the width of the bright CO-layer remains almost the same over the entire region we observed in contrast with the [\cii{}] and 8\micron{} emission, shown in Fig.~\ref{fig:obsemission} and \ref{fig:spitzer}, whose widths become broader up to a  factor of 1.5-2 in the south-eastern part of the observed region. Two of five massive YSOs, namely S2 and S10, are projected on the bright CO-layer, the other three massive YSOs are located outside the layer.  Several point sources, found by \cite{Deharveng_2009}, (see Fig.~\ref{fig:spitzer}), are located outside the CO-layer. Width of the whole molecular clump perpendicular to the ionization front is $\approx 0.4$~pc.

On the other hand, the map of the integrated intensity reveals also rather local phenomena, related to regions of star-forming activity. Several peaks of the integrated \co{} intensity appear towards YSOs but not towards the PDR's edge. Therefore, broadening of the \co{} lines towards the YSOs is responsible for the appearance of the integrated intensity peaks. The highest integrated intensity of \co{} coincides with the peak of the ATLASGAL 870~$\mu$m emission and the most massive YSO\,S2. There are three minor peaks of the \co{} emission towards YSOs\,S1, S10 and S39. There is one more massive YSO\,S9 in the map, but it does not demonstrate brightening of the \co{} emission.

\begin{figure*}
\includegraphics[width=0.99\columnwidth]{fig2a.pdf}
\includegraphics[width=0.99\columnwidth]{fig2b.pdf}
\caption{Left: map of the \co{} peak intensity in the RCW~120 PDR shown by colour scale. Contours show brightness of the [\cii] line emission at 20, 30 and 40~K. White crosses show positions of the \tco{} spectra shown in Fig.~\ref{fig:individual_spectra}, where position~1 corresponds to illuminated side of the PDR. Right: map of the \co{} integrated intensity shown by colour scale. The 870\,$\rm \mu$m contours for 0.4, 2.0 and 10.0 Jy/beam are shown by contours. The APEX beam at 691~GHz is shown by black circle. The black stars show the locations of YSOs from \citet{Figueira_2017} in both plots and in following figures.}
\label{fig:obsemission}
\end{figure*}

\begin{figure}
\includegraphics[width=0.9\columnwidth]{fig3.pdf}
\caption{Image at 8\micron{} and the map of the \co{} peak intensity are shown by colour and contours, respectively. The contours are shown for 30, 35 and 40~K\kms.
White triangles show YSOs from \citet{Deharveng_2009}. }
\label{fig:spitzer}
\end{figure}

The regions affected by the large-scale (related with the expanding \hii{} region) and local (related with the star-forming activity towards the YSOs) phenomena are clearly distinguishable in Fig.~\ref{fig:individual_spectra}, where we show individual \co{} and \tco{} spectra. The \co{} lines are single-peaked in positions~1-4 on the irradiated side of the PDR. Deeper to the molecular clump, the line profiles become double-peaked, less symmetric and demonstrate pronounced red and blue wings towards S2 (position~8). The irradiated side of the bright CO-layer demonstrates the narrowest width of the \co{} and \tco{} lines $\approx 4$\kms{} over the entire map including the area without YSOs deeper to the molecular clump in positions 11-18.

Local star formation reveals itself through the wings of the \co{} line clearly visible in positions 7-11. We find a narrow dip in the \co{} profiles at $-8$~\kms{}, which we associate with a self-absorption effect. The \tco{} line profiles are single-peaked everywhere except for the position~8, where velocities of the \co{} and \tco-dips on the double-peaked profiles are not the same, where the \tco{} dip is shifted to the red by 1~\kms{} and the \tco{} peak coincides with the \co-dip. Therefore, these dips can be caused by different factors: self-absorption for \co{} (also previously detected by \citet{Kirsanova_2019, Figueira_2020, Kabanovic_2022} for the (2--1) and (3--2) transitions, but shifted to the blue side for the (1--0) transitions in \citet{Anderson_2015}) and the gas infall for \tco, while the second statement requires further investigation using tracers of dense gas.

\begin{figure*}
    \centering
    \includegraphics[width=2.\columnwidth]{fig4.pdf}
    \caption{\co{} (black) and \tco{} (blue) spectra along the strip shown in Fig.~\ref{fig:obsemission}. The spectra are shown with the step of 3\arcsec{} from the north-east (position 1 at the offset $\Delta\alpha, \Delta\delta =$~21\arcsec,21\arcsec) to south-west (position 18 at the offset $\Delta\alpha, \Delta\delta =$~--30\arcsec,--30\arcsec). Towards S2, the \tco{} line is shown by red colour (position 8).}
    \label{fig:individual_spectra}
\end{figure*}

\subsection{Simulated \co{} and \tco{} line emission}\label{sec:simul}

In order to study the origin of the bright CO-layer, we compare the observed \co{} and \tco{} intensities in the layer with results of numerical simulations. Fig.~\ref{fig:radexmodel} shows the edge of the \hii{} region and surrounding PDR, where gas temperature and density change up to several orders. The dense layer of the neutral material, which has been accumulated around the \hii{} region by a shock wave, whose propagation preceded the expanding ionized gas. The shocked region contains the H/H$_2$ and C$^+$/C/CO transition. The mass of the shocked region is mostly contained in the gas where hydrogen and carbon are in the forms of H$_2$ and CO, respectively. Even in the region, where carbon is in the form of C$^+$, $n({\rm H_2})>n({\rm H})$ up to factor of few. Carbon becomes doubly ionized in the \hii{} region and distribution of C$^+$ traces the irradiated border of the PDR. The outer attenuated border is located inside of the shocked layer, there the extinction reaches 10 and higher values. The width of the chocked layer is $\approx 0.1$~pc.

\begin{figure}
\includegraphics[width=\columnwidth]{fig5.pdf}
\caption{Simulated (lines) and observed (colour rectangles and horizontal straight lines) properties of the RCW~120 PDR. Simulated physical conditions and chemical composition in the dense neutral layer around the \hii{} region obtained with the MARION model are shown on the two top panels. The ionizing star is located outside the left border of the panels in the beginning of the horizontal axe. The red rectangles and the red lines show the $\pm \sigma$ significance intervals and the best-fit solution of the non-LTE analysis with the observed and archival data (see Sec.~\ref{sec:analysis}). Simulated brightness of the \cii, CO and $^{13}$CO emission in different lines obtained with the RADEX software is shown in two bottom panels. Green and black horizontal colour bold lines and rectangles show the brightness and $\pm \sigma$ intervals for the archival $^{13}$CO(2--1) and (3--2) lines. The observed range of \co{} and \tco{} brightness are shown by the red rectangle. The \tco{} brightness used for simulations with RADEX is shown by the red horizontal line.}
\label{fig:radexmodel}
\end{figure}

It is seen from Fig.~\ref{fig:radexmodel}, that spatial distribution of brightness temperatures for the CO and $^{13}$CO (2--1) and (3--2) line emission does not allow to resolve the thickness of the shocked layer. The peaks of the (2--1) transitions are shifted outside the PDR, the peak widths are two times broader than the layer, and the contrast between the peak and emission from undisturbed molecular gas is only 20-50\%. The (3--2) transitions better trace the shocked layer, while the widths of the peaks are still broader and the contrast reaches only a factor of 3. Only the (6--5) line emission reaches its maximum exactly at the densest part of the shocked layer and has zero-to-zero width exactly the same as the width of the shocked layer. The peak of the simulated \cii{} emission is shifted to the ionizing star for less than the APEX beamsize at the 690~GHz. Simulated brightness of the \co{} and \tco{} lies in the interval and agrees with the low limit of the observed values, respectively, see Fig.~\ref{fig:obsemission} The simulated \cii{} also lies in the observed interval of values, see contours in Fig.~\ref{fig:obsemission}. Simulated $^{13}$CO(2--1) and (3--2) lines intersect the ranges of the line brightness taken from \citet{Kirsanova_2019}.

Comparing the view of the bright CO-layer in Fig.~\ref{fig:obsemission} and results of the simulations in Fig.~\ref{fig:radexmodel}, we relate this layer with the shocked dense neutral material, which has been shovelled up on the border of the ionized region during hundreds of thousands of years. The shocked layer represents large-scale structure, related with evolution of the \hii{} region. In RCW~120, we see the \co{} emission also outside the shocked layer, probably due to local heating from embedded YSOs. Below we show how the shocked layer is displayed in the kinematic structure  of the observed region.

\section{Physical conditions in molecular gas}\label{sec:analysis}

In this section we analyse radial distribution of excitation conditions for the \co{} and \tco{} lines using the LTE approach and also combine these data with available archival data for the non-LTE analysis in the most interesting directions of the observed region.

\subsection{LTE}\label{sec:lte}

We show in Fig.~\ref{fig:LTEanalysis} (top panel) radial profiles of the \co{} peak brightness and integrated intensity, taken perpendicular to the PDR along the \tco{} strip. Spatial difference between the maxima of the peak and integrated intensities $\approx9$\arcsec, i.e. about the size of the telescope beam. Spatial behaviour of the \tco{} peak intensities qualitatively resembles the \co{} emission with the sharp/smooth decreasing on the inner/outer sides of the PDR. However, the \tco{} integrated intensity shows almost symmetrical spatial distribution around the YSO~2 which can be related to its lower optical depth. Comparing the observed and simulated radial distributions in Fig.~\ref{fig:radexmodel}, we note that both the \tco{} distributions are symmetric. However, there is no smooth decrease of the simulated \co{} emission on the outer side of the shocked layer. We relate the enhancement of the observed \co{} emission in positions 11-18 with local star-forming activity in the region, which is not included into our simulations.

With both the \co{} and \tco{} lines, along the same strip in molecular cloud, we estimate the optical depth of the \co{} line and the CO column density using an LTE~approach, explicitly described by \citet{Mangum2015},  see Eq.~(79) therein.  This approach assumes the same constant excitation temperature ($T_{\rm ex}$) for \co{} and \tco{} along the line of sight. For the (6--5) transition we used the energy of the upper level $E_{\rm u}=116.2$~K, rotation constant $B_0=55101.014\times10^6$~Hz, and dipole moment $\mu = 0.1$~Debye. Results of the LTE~analysis: optical depth of the \co{} line $\tau$, excitation temperature $T_{\rm ex}$ and CO column density $N_{\rm CO}$ are shown in Fig.~\ref{fig:LTEanalysis}. In order to estimate uncertainties of $T_{\rm ex}$, $\tau$ and $N_{\rm CO}$, we varied integrated intensities of the \co{} and \tco{} lines as well as the \tco{} brightness temperature within their $1\sigma$ intervals. Repeating the procedure 100 times, we find the average values of these parameters with their standard deviations.

The \co{} lines are optically thick in all positions where we detect the \tco{} emission with the \co{} optical depth $\tau \approx 18-20$ in the direction of S2 and $10 \leq \tau \leq 20$ in the direction of the PDR. Dividing the $\tau$ value by the $^{12}$C/$^{13}$C ratio $=61$, suitable for the galactocentric distance of RCW~120~\citep{Wilson_1999}, we find optically thin \tco{} line along the strip even in the direction of the YSO. The value of $T_{\rm ex}$ does not exceed 50~K and has almost flat radial profile along the strip within the interval of $40-50$~K. As we work in the LTE~approximation, we estimate thermal width of the \co{} line using the $T_{\rm ex}$ value and find it $\leq 0.5$~K. Optical depth of the \co{} line also contributes to the broadening by a factor of $\approx {\rm log}(\tau) \approx 2-3$, i.~e. up to 1\kms{}. Totally, thermal and depth-related broadening provide less than 25\% of the observed line widths. Therefore, the widths of both \co{} and \tco{} lines from Fig.~\ref{fig:individual_spectra} are non-thermal, but the width of the self-absorption feature is thermal. Therefore, the self-absorption of these relatively high excitation lines ($E_{\rm u} > 100$~K) can be caused by cool gas between RCW~120 and the observer.

CO column density distribution along the strip has two maximal values of $N_{\rm CO} \approx 2\times 10^{19}$~cm$^{-2}$ in the direction of the PDR and the YSO S2, respectively (spectra 1, 2 and 8 in Fig.~\ref{fig:individual_spectra}).  Using values of hydrogen column density from the ViaLactea survey \citep[based on {\it Herschel} data, see][]{Marsh_2017}, we determine relative abundance of CO in the bright CO-layer and other directions along the strip and find it $\sim 10^{-4}$. The CO/H$_2$ ratio is close to the elemental abundance of carbon, H$_2$ and CO are well mixed with each other in the PDR and in the remaining part of the molecular clump also. Therefore, the CO and H$_2$ dissociation fronts should be situated closer to the ionizing star than position~1 in Fig.~\ref{fig:obsemission}. While the ViaLactea maps may underestimate hydrogen column density, the uncertainty related to the {\it Herschel} fluxes does not significantly affect the densest regions, see, e.~g. a comparison made by \citet{2021MNRAS.506.4447L}.

\begin{figure}
    \centering
    \includegraphics[width=\columnwidth]{fig6.pdf}
    \caption{Integrated and peak intensities of the CO(6--5) and $^{13}$CO(6--5) emission (two top panels) as well as the results of the LTE analysis along the cut. Position 8 corresponds to the direction to the Core~2 YSO. Grey rectangles at the bottom panel correspond to the ranges of $N_{\rm CO}$ from the non-LTE analysis.}
    \label{fig:LTEanalysis}
\end{figure}

\subsection{non-LTE}\label{sec:nonlte}

While straightforward LTE analysis allows estimating gas temperature ($T_{\rm gas}$) in molecular gas, it doesn't give any information about the gas number density ($n_{\rm H_2}$). Therefore, we combine the \tco{} line emission data from the present study and the $^{13}$CO(2--1) and $^{13}$CO(3--2) data from \citet{Kirsanova_2019}, to estimate physical conditions in three different regions in RCW~120. Namely, towards the S2 YSO, to the PDR layer (position with the offset $\Delta \alpha, \Delta\delta = 20$\arcsec,20\arcsec{}, between positions 1 and 2 in Fig.~\ref{fig:obsemission}), and towards molecular cloud ($\Delta \alpha, \Delta\delta = -20$\arcsec,--20\arcsec{}, between positions 15 and 16), all positions are given relatively to the S2~YSO at $\alpha=17\rm ^h$12$\rm ^m$08.700$\rm ^s$ and $\delta=-38^\circ$30\arcmin46.40\arcsec (J2000). There are no YSOs in the PDR and MC directions, therefore we can obtain parameters of molecular gas without contamination of any activity related to star formation. We fixed the widths of all the CO lines to 4.4\kms{} and background temperature to 2.7~K in order to calculate non-LTE models with RADEX software on a grid of different $T_{\rm gas}$ (from 10 to 200~K divided by 100 intervals), $n_{\rm H_2}$ ($10^3 -10^7$~cm$^{-3}$, 100 intervals), $N_{\rm ^{13}CO}$ ($10^{14}-10^{18}$~cm$^{-2}$, 100 intervals). The best-fit results and $\pm \sigma$ significance intervals, found with the $\chi^2$-test \citep[][]{wall_jenkins_2003} are shown in Table~\ref{tab:nonLTE}. In order to estimate dependence of the $\chi^2$ minimum on the noise level of the various $^{13}$CO lines, we varied their integrated intensities within the $1\sigma$ levels: 0.3, 0.1 and 1.5~K for $^{13}$CO(2--1), $^{13}$CO(3--2) and \tco, respectively. Repeating the procedure by 100 times, we found the average minimum of the $\chi^2$ value and corresponding average parameters with their standard deviations. For the YSO model, the average minimum $T_{\rm gas}$ and $n_{\rm H_2}$ with their standard deviations are shown in Fig.~\ref{fig:nonLTEanalysis}. Comparison of the error bars with the shape of the $\chi^2$ dependency of the $T_{\rm gas}$ and $n_{\rm H_2}$ values shows that the quality of the observational data does not affect on the best-fit parameters, while the degeneracy of the best-fit parameters is significant due to the $^{13}$CO line excitation conditions. However, we become convinced that the solution for the minimum is steady.

We find that the $N_{\rm ^{13}CO}$ value is determined with an accuracy of 30-60\%, while the $\pm \sigma$ significance intervals are much broader for $T_{\rm gas}$ and $n_{\rm H_2}$. Considering only those $T_{\rm gas}$ and $n_{\rm H_2}$, which corresponds to the best-fit $N_{\rm ^{13}CO}$ values, we find almost the same intervals, those are shown in Fig.~\ref{fig:nonLTEanalysis} for the YSO position (the $\chi^2$ diagrams for the PDR and MC positions have similar shape).  The value of $T_{\rm gas}$ from non-LTE analysis agrees within a factor of two with $T_{\rm ex}$ values from the LTE analysis in the PDR and MC positions, but the minimum $\chi^2$ value was found at $T_{\rm gas} = 124$~K towards the YSO. While the values of $N_{\rm CO}$ from LTE and non-LTE analysis are also in agreement within the uncertainty intervals (see the bottom panel in Fig.~\ref{fig:LTEanalysis}, where we show $N_{\rm CO} = 61\times N_{\rm ^{13}CO}$), the non-LTE value is lower by an order of magnitude towards S2. Therefore, the non-LTE effects of the line excitation are important towards the S2 YSO, but the LTE approximation is valid for the physical conditions in the MC position.  The gas temperature $>100$\,K, found in S2, agrees with the results by \citet{Kirsanova_2021}, who found hot gas towards the YSO.

The non-LTE intervals for the $n_{\rm H_2}$ and $T_{\rm gas}$ values at the PDR position agrees also with the simulated values in the shocked material, see Fig.~\ref{fig:radexmodel}. This agreement confirms that the bright CO-layer is the shocked gas indeed. The best-fit $n_{\rm H_2}$ value in the PDR position is by 2-2.5 orders of magnitude higher than that in the YSO and MC positions. We explain this fact by compactness of dense material in the direction of the YSO and relatively large beam size of our observations. The minimum non-thermal line width of the \co{} line together with the high density of the PDR also indicate that the bright CO-layer might represent the gas where internal chaotic motions were suppressed by the shock.

\begin{table}
\centering
\begin{tabular}{c|c|c|c}
\hline
           & $T_{\rm gas}$     & $n_{\rm H_2}$ & $N_{\rm ^{13}CO}$    \\
           &  (K)              & ($10^4$~cm$^{-3}$)   &($10^{16}$~cm$^{-2}$)        \\
\hline
PDR        &  $50_{37}^{200}$  & $950_{1.0}^{1000}$ &  $0.8_{0.6}^{1.1}$ \\
\vspace{0.025cm}\\
Core~2 YSO & $124_{40}^{200}$ & $1.3_{0.6}^{1000}$ &  $4.7_{4.3}^{6.1}$\\
\vspace{0.025cm}\\
MC         &  $64_{22}^{200}$ & $1.5_{0.2}^{1000}$ &  $1.7_{1.3}^{2.8}$  \\
\hline
\end{tabular}
\caption{The best-fit results and $\pm \sigma$ significance intervals of non-LTE analysis for the Core~2 YSO, PDR and molecular cloud.}
\label{tab:nonLTE}
\end{table}

\begin{figure}
    \centering
    \includegraphics[width=0.99\columnwidth]{fig7.pdf}
        \caption{Grid of the $^{13}$CO RADEX models for different gas temperatures and densities at the best-fit $N_{\rm ^{13}CO}=4.7\times 10^{16}$~cm$^{-2}$ for the S2 YSO position. Colour shows $\chi^2$ where values are decreasing towards dark red.}
    \label{fig:nonLTEanalysis}
\end{figure}

\section{Kinematics of the molecular gas}\label{sec:kinematics}

Position-velocity (pv) diagrams in Fig.~\ref{fig:pv_perpendicular}, made parallel and perpendicular to the ionization front, show complex structure of the observed region. Making the cuts perpendicular to the ionization front, we clearly see the bright CO-layer with narrow \co{} lines, which we relate to the shocked layer. This gas is unperturbed by the embedded YSOs, see e.~g. the diagram~1p at the offset~$\approx 30$\arcsec. The lines become broader at the larger offsets $\approx 50-70$\arcsec{} as we move away from the PDR to the molecular clump. All the observed line widths are non-thermal (see analysis of physical parameters in Sec.~\ref{sec:analysis}), therefore we suggest that the velocity dispersion can be decreased in the shocked layer due to compression (and higher turbulence decay) and star-forming activity leads to the broadening of the lines outside the layer. The pv~diagram~2p demonstrate local gas kinematics related to star-forming activity in the S2~YSO, namely broad lines with wings at the offset~$\approx 30-50$\arcsec{} and less broad at the higher offsets deeper into molecular clump. We note a narrow dark line at $V_{\rm lsr} =-7.5$\kms{}, which we relate to self-absorption effect caused by the large-scale foreground material extended over RCW~120 and described in Sec.~\ref{sec:intro}. Stratified structure of PDR and a transition from atomic to molecular gas can be seen from comparison of the \co{} and archival [\cii] pv~diagrams, also shown in Fig.~\ref{fig:pv_perpendicular}. We find the [\cii] peak closer to the ionization front than the \co{} peak at the pv~diagram~1p. However, the [\cii] and \co{} peaks coincide at diagram~2p. We will discuss properties of the C$^+$/CO transition of the PDR in Sec.~\ref{sec:discussion}.

\begin{figure*}
    \centering
    \includegraphics[width=0.85\columnwidth]{fig8a.pdf}
    \includegraphics[width=0.59\columnwidth]{fig8b.pdf}
    \includegraphics[width=0.59\columnwidth]{fig8c}\\
    \includegraphics[width=\columnwidth]{fig8d.pdf}
    \includegraphics[width=\columnwidth]{fig8e.pdf}\\
    \includegraphics[width=\columnwidth]{fig8f.pdf}
    \includegraphics[width=\columnwidth]{fig8g.pdf}
    \caption{Pv~diagrams of the CO(6--5) line emission. Top row: map of the integrated \co{} emission where red lines show directions of the pv~diagrams. Pv~diagrams for the \co{} (color) and [\cii] lines (white contours), taken perpendicular to the ionization front are given on two right panels (1p and 2p). Middle and bottom rows: pv~diagrams taken parallel to the ionization front (1--4). Black dashed lines show positions of YSOs on the pv~diagrams, names of those are given in black.}
    \label{fig:pv_perpendicular}
\end{figure*}

Pv~diagrams, made parallel to the ionization front, distinguish regions of the large-scale shocked layer and dense molecular clump. The diagrams~1 and 2 show a straight line at --8\kms{} which makes a red-shifted arch up to --2\kms{} at the offsets~60--110\arcsec. The arch becomes double-sided in diagrams~3 and 4 between the same offsets. The broadest \co{} lines appear in positions of YSOs. Comparing the diagrams~3 and 4 with the line profiles in Fig.~\ref{fig:individual_spectra}, we relate these broad lines to outflows to the red and blue sides, accompanying the star formation process towards the YSOs. Therefore, from these pv~diagrams we distinguish two regions: the first one is regular structure related to the large-scale shocked layer from the expanding RCW~120 (at the offsets $<60$\arcsec{} and $>110$\arcsec) and the second one related to star-forming regions in the dense clump.

Outflow candidates, detected by us in the present study, do not look like those that were found previously by \citet{Figueira_2020} with low excitation CO(3--2) line. Therefore, we show the candidates in Fig.~\ref{fig:outflowsreal} considering the same velocity intervals as it was done for the CO(3--2) line. We find not one but several candidates using two times higher angular resolution. The first candidate, related with the S2~YSO, appears as an outflow oriented along the line of sight as the red and blue lobes almost coincide. Different geometry visible with the higher excitation lines can be related with the complex structure of the outflow near and far from the exciting source, traced by the (6--5) and (3--2) transitions, respectively. We find intersecting red and blue patches toward the S1~YSO where the blue-shifted part is much brighter than the red one. The red wings of methanol lines were seen previously by \citet{Kirsanova_2021}, therefore we do not have doubts about the outflow activity there. We deduced from emission maps of CH$_3$OH, SiO and DCO$^+$ molecules (Plakitina et al., in prep.), that only red and blue patches around S1 and S2 are real outflows, but the other ones visible between S9, S10 and S39 are parts of complex kinematic structure of the region.

\begin{figure}
    \centering
    \includegraphics[width=\columnwidth]{fig9.pdf}
        \caption{Channel maps of the \co{} emission around RCW~120. There are three velocity intervals in this map: $V_{\rm lsr} < -9$ (blue contours), $-9 < V_{\rm lsr} < -4$ (middle, shown by greyscale) and $V_{\rm lsr} > -4$~\kms{} (red contours). The contours are shown from 30 to 90~K~\kms{} through 10~K~\kms.}
    \label{fig:outflowsreal}
\end{figure}

\section{Discussion}\label{sec:discussion}

We know that stellar wind \citep{Luisi_2021} and ionized gas \citep[][]{Sanchez-Cruces_2018} expel all neutral material and produce dense expanding PDR around the bubble. The appearance of a dense layer, swiped by the shock wave, in the neutral side of PDR accompanies the expansion \citep[][see also calculations by e.g.~\citet{Hosokawa_2005, Kirsanova_2009, Akimkin_2015,  2018arXiv180101547B}]{Spitzer_1978}. We associate our bright CO-layer with the shocked molecular layer, moving away from the ionizing star, as we have shown above. While the bubble and the PDR resembles a sphere, the molecular region certainly has different geometry and resembles a flattened envelope oriented face-on which can be modelled in the plane-parallel approach.

Abundance of CO in the shocked layer agrees with the elemental value for this part of the Galaxy, it means that carbon is locked in this gas-phase CO. Since the position of the H$_2$ dissociation front normally coincides with the bright 8\micron{} emission from PAHs \citep[e.~g.][]{2010ApJ...725..159F, 2021ApJ...919...27K}, we conclude that the CO and H$_2$ dissociation fronts are situated on the inner border of the bright \co{} layer. The merged fronts appear as a natural consequence of the ongoing propagation of the dissociation fronts through the dense molecular cloud \citep[see e.~g. simulations by][]{Storzer_1998, Hosokawa_2005, Kirsanova_2019b}: the denser the gas the closer the fronts. The pv~diagrams from Fig.~\ref{fig:pv_perpendicular}, taken perpendicular to the ionization front, confirm the merging of the H$_2$ and CO dissociation fronts in the dense material. For instance, comparing the diagram~1p and 2p, taken outside and through the dense material, respectively, we find different separation between the [\cii] and \co{} peaks. The peaks do not coincide in the diagram~1p, but they merge in the diagram~2p. Taking into account divergence of the \co{}, [\cii] and 8~\micron{} peaks in the south-eastern part of the observed region, we suggest that the CO and H$_2$ dissociation fronts might be separated there.

The shocked molecular gas appears as the most regular structure in our maps of the line emission in Fig.~\ref{fig:obsemission} and pv~diagrams in Fig.~\ref{fig:pv_perpendicular}. While the line width is still non-thermal, its value is about a factor of 2 lower in the shocked layer than in the molecular clump. Significant broadening of the molecular lines occurs near YSOs and is related to outflows. The shock does not disperse the dense clump unlike the outflows. This scenario looks similar to the recent findings by \citet{Kavak_2022} in the Orion region and can be widespread around O-type stars surrounded by younger star-forming regions. Comparing the positions of YSOs found by \citet{Deharveng_2009, Figueira_2017} with the location of the dense shocked layer (see Fig.~\ref{fig:spitzer}) we agree with conclusion by \citet{Figueira_2020} that the YSOs were pre-existed before the shock wave from RCW~120 reached the molecular clump.

\section{Conclusions}\label{sec:conclustion}

In this study, we made spatially and velocity-resolved observations of the RCW~120 PDR and nearby molecular gas with \co{} and \tco{} lines and found a bright CO-emitting layer towards the PDR. We simulated physical conditions and emission of several CO and C+ lines in the RCW~120 PDR and found reasonable agreement with the observed values. Based on this agreement, we related the CO-bright layer with shocked molecular gas moving away from the ionizing star due to expansion of \hii{} region. While the shock itself is not visible, we found its impact on the neutral material around RCW~120 in our \co{} map. We distinguished between large-scale structures and kinematical features such as the shocked gas and local ones such as dense environments of embedded protostars and outflows. We found the shocked layer as the most regular structure on the \co{} map and in the velocity space, whereas the gas around YSOs was dispersed by the outflows.

\section*{Acknowledgements}

We are thankful to S.~V.~Salii and K.~V.~Plakitina for fruitful discussions. We also thank unknown referee for his/her very relevant comments.

Based on observations with the Atacama Pathfinder EXperiment (APEX) telescope. APEX is a collaboration between the Max Planck Institute for Radio Astronomy, the European Southern Observatory, and the Onsala Space Observatory. Swedish observations on APEX are supported through Swedish Research Council grant No 2017-00648.

M.~S.~K. and Ya.~N.~P. were supported by RSCF, project number 21-12-00373. D.~A.~S. acknowledges financial support by the Deutsche Forschungsgemeinschaft through SPP 1833: "Building a Habitable Earth" (SE 1962/6-1). A.~F.~P. acknowledges the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038.

\section*{Data Availability}

Calibrated data on \co{} and \tco{} emission generated in the study can be found in the ESO Archive (projects O-0103.F-9301A-2020 and O-0107.F-9318A-2021). Results of the calculations with MARION are available in Zenodo, at https://zenodo.org/record/7447109.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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Downloads - is the total amount of content updates requested by your app users from our servers - only unique devices are calculated (the numbers provided by iBuildApp.com may differ from the download stats provided by app store).
Apps - is the total number of apps/projects created under one reseller account.
You don't need any technical infrastructure in order to run the platform - it is in the cloud. In addition, the platform is highly secure and meeting all current industry standards.
The reseller program provides promotional and marketing tools such as ability to integrate coupons, access to analytic modules that show analysis, trends and benefits to your customers.
The core of our Reseller program is to help you generate revenues on a recurring basis. You resell apps monthly. As a Reseller you have a wholesale unit price per package, per month.
If you need any help with your Reseller site customization or you've got troubles while creating your apps, then you can sign up with our Premium Reseller Support Plan.
(CSS is a style sheet language used for describing the presentation semantics (the look and formatting) of a document written in a markup language).
Poedit is cross-platform gettext catalogs (.po files) editor. It is built with wxWidgets toolkit and can run on any platform supported by it (although it was only tested on Unix with GTK+ and Windows).