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Iran and the western-manufactured hijab protests
Attempts to cast imperialist countries as champtions of women's rights are laughable to anyone familiar with the declining position of women in the west.
The stirring up and coverage of an allegedly widespread protest movement (even 'revolution') against the hijab in Iran, supposedly in defence of the rights of women, is a classic example of imperialist media lies and regime-change operations. This image, for example, is presented on a page that purports to show the protests 'in pictures', but this picture and several others shown there are actually from sympathy protests (shot up close so as to conceal the small scale) in imperialist countries like the USA and Germany. Moreover, all the banners are written primarily in English, for consumption by western audiences. Another non-reported aspect is that most of the protests that did take place in Iran were in areas where Kurdish groups aligned with the USA are active and have been trying to turn Mahsa's tragic death into an ethnic issue.
The western media are harping on relentlessly about great anti-hijab protests which they assure us are happening all over Iran, and which they claime are being met with ever more violent repression by a 'vicious and violent regime'. The nail that they are trying to hang this deceitful web of lies on is the story of Mahsa Amini, a 22-year-old Kurdish woman.
The known facts – of the sad death of this young woman – are as follows: during a shopping trip to Tehran with her family, she had emerged from a metro station and entered Talaqani park, where she was walking with three female and two male relatives, including her brother Ashkan. The group was approached by members of the 'morality police', who said she was in breach of the islamic dress code. Two of the women were given warnings, but Amini, despite pleas from her aunt that she was from out of town, the dress code being much less observed in many smaller towns and rural areas, was directed into a van to be taken to a police station for a correction lesson.
These 'lessons' are usually a 60-minute lecture before being released. A video recording from the station released by the police shows Mahsa Amini standing alone, collapsing onto a chair and then to the floor. She had had a stroke or a heart attack, and died before the ambulance got her to hospital.
This was, of course, an unfortunate and terrible occurrence, but it is one that does happen from time to time to people anywhere in the world. Some of the grieving family have blamed the 'morality police' for Mahsa's death, and the increased stress of the incident may well have been a trigger in some way, but to someone who is unknowingly especially vulnerable, many things could have contributed – the shopping trip to the big city, the noise and bustle even. Clearly something, even if it might not have been greatly stressful for a person in good health, increased the likelihood of this tragedy for Mahsa.
Western forces, media, NGOs, spy groups and the rest all grabbed at the story and have twisted and 'gilded' it beyond any recognition, doing their level best to turn it into a tale of state terror by the Iranian government and hoping thereby to rouse an anti-government 'popular' uprising throughout Iran.
All the usual suspects have been given the usual amount of airtime on imperialist media outfits to try to convince the world that a counter-revolution (they would call it a revolution, of course) has flared up, and that blood was running on the streets all over Iran as the masses rise up against a hated islamic dictatorship that is resorting to extreme violence to keep the people down.
Of course, nothing of the sort has happened. The masses support their government for the most part, are proud of their country's achievements, and the living standards of the majority are deemed by them to be generally good.
Morality dress codes come and go in all societies and Iran is not alone in this. We know from hundreds of ordinary everyday bloggers in Iran, people who daily record and transmit pictures of their streets and communities, that riot situations have been very rare. Those few that have taken place have been manufactured by western interests.
In fact, across Iran, even before Mahsa's tragic passing, observance of the dress codes by Iranian women is not universally adhered to, and there is little or no reaction from the state.
The Iranian people have their own way of influencing their government. The so-called 'morality police' have been disbanded and the whole matter is history as far as most Iranians are concerned. However, those who seek to bring Iran down, who want to end its anti-imperialist stance and its friendships with Cuba, Venezuela, China, Russia etc, will try to keep this story alive in order justify their interference in Iran's social and economic affairs.
"Never in my 14 years working on human rights advocacy have I witnessed such disillusionment with, and opposition to, the Islamic Republic regime," said Nazanin Boniadi, a British-Iranian actor and Amnesty International ambassador. "While Iran has become accustomed to mass protests every decade, neither the student protests of 1999 nor the green movement of 2009, or even more recently the November 2019 protests, compare in fervour or magnitude to the current protests."
Boniadi added: "The most unprecedented part is that the protests have been female-led." Playing to the ultra-left gallery that is always there to promote imperialism's interests as 'revolutionary', she continued: "The movement's slogan 'Women, life and freedom' is antithetical to the Islamic Republic, which has built itself on being anti-woman, pro-martyrdom and repressive. This uprising is not just about draconian dress codes. The compulsory hijab has simply become a symbol of a wider Iranian women's struggle."
Revealing the real point of imperialism's interest in women's issues, fellow imperialist stooge Kasra Aarabi, an Iran analyst at the Institute for Global Change, described the mood in the country as 'revolutionary'. "The people that speak to me believe they are in the middle of a revolution and will not back down. One way or another, this is the beginning of the end of the regime. This is not about reform. This is about regime change."
Amongst the endless list of inane celebrity wannabes who have jumped on this bandwangon in order to promote themselves is Donya Dadrasan, an Iranian popstar who lives in Australia, and who has poured out invective worthy of a Sun journalist against the morality police on Instagram. Meanwhile, a quite staggering number of cretins have stood pouting into their camera lenses while publicly cutting their own hair 'in solidarity with Mahsa'.
As in all things, the imperialists will try to use any event, any tragedy, in order to launch an attack on countries which, like Iran, will not follow the dictates of imperialism. Our job is to look past all the blather and find the real aim of the western media and its hypocritical narrative.
When French male gendarmes were stripping muslim women on French beaches of the islamic beachwear that kept them covered, how many of these ink-flingers raised even a whimper in opposition?
In our view, Iran would do well to do away not only with the 'morality police' but also with the mandatory dress code for women, which, while doing no good to Iran, provides imperialism and its flunkeys with yet another pretext for poking their snouts into Iranian internal affairs, which are the sole preserve of the Iranian people.
Divide and rule
Malthusianism is alive and well as feminists celebrate declining birth rate
JK Rowling's stance against the thought police
Women in the victory over fascism
Deborah Lavin: Early feminism, bourgeois and proletarian
The women's movement in Britain
Iranian professor: 'Israel is in no position to wage war against Iran'
A critique of the CPB's 'Britain's Road to Socialism' in the 21st century, pt 3
Comrade Lauren: 'Identity politics divide workers'
October 100: Women's liberation
Since they cannot admit to a solution lying outside of capitalist production relations, 'women's rights' advocates are reduced to prettifying their chains.
2 Sep 2022, Proletarian
The author's brave stance in defence of reality must be defended, and her hysterical detractors exposed as the reactionary bullies they are.
Without the brave and tireless efforts of women across the USSR and Europe, vanquishing the enemy would have been impossible.
21 May 2020, Proletarian
What did the early Marxists think about birth control and women's rights? How did their views differ from those of the liberal feminists?
4 Apr 2020,
Why is the women's movement in this country so totally unappealing to working-class women? Why do Marxists oppose 'feminism'?
16 Mar 2019,
The days when Israel's firepower and US backing could cow the rest of the region into submission are gone.
22 Aug 2021,
Eclectic and utopian, the CPB's programme is full of pious wishes but its authors don't seem to have the first clue about the realities of the state or of class war.
Women's liberation is a question for all of us; a key part of the working-class struggle for socialism.
8 Mar 2021,
16 Mar 2019, Proletarian TV
The October Revolution changed forever the perception and accepted role of women in society, showing the way to complete emancipation and equality.
5 Oct 2018, Proletarian TV


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All Things To Do In San Francisco Explore Cultural & Sightseeing Neighborhoods
Castro Mission Tour
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Explore Castro Mission Loop, one of the San Francisco's oldest areas, for an informative walking tour
See Liberty Hill, the oldest building in the city, murals, Victorian architecture, and a buried lagoon
Gain knowledge about the history of this hotbed of American culture
Take a relaxing, scenic 3.4 mile walk through one of the most famous neighborhoods in San Francisco
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Visit the rich history and culture of Castro Mission Loop's LGBTQ+ community, the nightlife with a Latino flair, and the iconic Victorian Architecture.
Your next stop is an oldest building in the City and namesake of the Mission District: Mission Dolores. At the Mission, you'll learn old Spanish-California stories before you dive into one of the most happening neighborhoods in America. Known for its Latin roots, mural-lined streets, and eccentric nightlife, the Mission is the place to be. Take note of the craft cocktail bars, authentic Mission-style taquerias, and techno clubs to plan an unforgettable evening after the walking tour. Between the Castro and the Mission, two and a half hours won't seem like enough to soak in these sensational San Francisco Districts.
Note: While leisurely, this tour involves many steps, which can be challenging. The exact meeting location will be provided upon confirmation of booking.
Price $50.00 per guest
Duration / Session 2.5 hours
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You've formed a company. You've built your product. You've validated the market and there has been early interest from a small number of potential clients.
You have a vague idea of how much you should charge for your product. In fact, if you have a firm idea, or you have spent hours on excel working on varying permutations and pricing models – drop it, keep an open mind.
You core staff are working on developing the product, looking after early stage users.
Your leadership team have done a great job evangelising and promoting your business. Investors and perhaps government agencies have chipped in to fund the venture.
An actual product that could be used by paying customers (but that's ok, we can sell products that provide enough, instead of everything).
Someone in the team who will be fully focussed on sales (which we means not all the team can be working on product building, for a change).
The most basic marketing materials (because your website and wonderful CEO is enough.. nope).
A sales deck, a proposal template or even some contract paperwork.
So how do you land your first customer? So let's keep this simple(ish). How do you start selling? Where do you start?
Don't hire anyone to do sales yet.Founders and their team should try to make the first sale(s) yourself. Founders should make the first sales, before they bring in someone to do it (unless you have the good fortune of having a co-founder who has a background in sales, in which case — you are very lucky). You don't have to be experienced in sales to get the ball rolling on your company's first few sales, but give it a go.
Don't distract yourself with tool and gadgets.You don't need a CRM just yet, or marketing automation or …anything. Don't worry about that stuff for the moment. When you need it, address it. What's that old saying about cart before horse). How many startups waste time and money getting all the processes and tools in place first. Don't get distracted.
Know who you are selling to, and what problems your product solves. (Well at this stage, I would hope that you are past this stage). But ask, how will they buy, what problem does your product solve, what are the probable prices for your product. These things can change as you start to gain traction, but you can't start selling if you don't have a particular kind of prospect in mind, and how it will help them. Again, this should go without saying.
Ask for referrals.Use your network. Tell your friends, family, associates, colleagues. Tell everyone you know, professionally and otherwise, about your product. You can ask them to buy if you want to, but it may be better to just ask for referrals. Tell people about your product, what problems it solves, who is for, and ask if they know anyone that it might be a fit for.
Your momma isn't your test market, but you will probably know someone – who knows someone.
You might get a referral or two – and you will get practice selling to people. As long as you are selling – which is more about listening and asking questions, that it is telling.
Build a short list of ideal customers.Do you know who they are? Create a list. You don't need a CRM just yet, a spreadsheet will do. Email them, call them, visit them. Meet them and talk, and listen. Because the more you interact with them, you will slowly realise that your ideal list will become a simple list of prospects. Nothing ideal about them at all – simply entities who may or may not purchase your product.
Do whatever it takes to win your first customer.There is nothing better than the feeling of bagging your fist client, whether you have met them and clinched a deal or they visit your website and make a purchase. Be flexible with your first customers and do what it takes to win the deal. You nee them more than they need you. Remember, they are also taking a risk on a new product in the market, so reduce the risks wherever you can to give them the peace of mind, and your team see the relationship work, and revenue roll in. Remember, these early stage customers are going to give you feedback, they are going to tell you that it isn't quite perfect. So listen. Likewise, some early stage customers will not contact you and tell you the problems they are experiencing. Some early clients will not find the time to tell you what is wrong – so keep in touch with them. Contact them, ask them how they are getting on.
We're not trying to oversimplify sales.
Sales is an art, and it's a science, it requires tremendous skill and importantly resilience. As a salesperson you will have to accept failures, no interest, criticism and vulnerability. Far from the cocooned world of the startup in the stages of product development and fund raising.
If you need help assessing your current sales scenario then contact us today.


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Q: A few classes versus 20 classes? A question about bloat In evaluating the work of an outsourcing company, I have found that they have a propensity for dividing work into as many classes as possible, each one being testable. In some ways this seems commendable, but they are taking it to an extreme and no one seems able to control them.
Recently I found what should have been a simple UI piece that I would have implemented as at most 3 classes (one for data, one for controller, one for view), they had in fact broken up into some 20 classes (e.g. base class and multiple derived classes) and protocols, requiring in the end about 70 source files (Objective C .m files and .h headers) which included a test for each and every part, even the tiniest piece. Their code, despite the elaborate testing code, barely works and is constantly breaking.
They justify this with vague talk about SOLID and/or the "massive class" problem.
This code is already written. No one but them was allowed to design it. I can criticize implementation, but not really influence design.
So what is a good strategy, other than seeking better employment, for dealing with Outsourcing Companies Gone Wild where their numerous engineers  expand simple projects as much as possible and as long as possible in this way, rendering them complicated and vast?

A: Given problem x how can I say 20 is wrong and 3 is right?
Here's how:
On a good day my brain can hold 7 things at a time. That's it. No more. Sometimes it's only 5.
So 20 is to much. Don't care what x is.
However, 4 abstractions with 5 classes hiding behind each is fine. And yeah. That is still 20. Likely more.
What I'm saying is the numbers matter but so does the organization. If these guys are going nuts with small classes but doing nothing to organize them then they're causing a real problem. It's not just that you're not used to the style. It's that they're asking you to remember more than 7 things at once.
This is a valid style. Be careful not to come off as simply against it. Instead emphasize the need for trustworthy abstractions to improve readability. If you have to dive into an abstraction to understand it, it's not working.
They decided to break things down this small. It's on them to put it all together in a way that makes sense.

A: Without see the code is hard to tell if they are doing a good or bad job.
But normally is a good idea break the code in tiny classes. This strategy is very common when you are not sure about the better organization of the code: what classes you really need, how they will be organized, the domain knowledge is not good yet, etc.
Maybe you can argue something in this line to convince the rest of the team that some classes makes more sense to be only one class now. There is an article about that by Martin Fowler .

Their code, despite the elaborate testing code, barely works and is constantly breaking.

This is not necessarily a problem from the tiny classes strategy. Maybe the project need some integration tests to see if the all this classes are working well together.

A: Answer to your question cannot be binary yes or no. It depends. It depends whether those 20 classes are result of class explosion due to bad design or is because of well thought of structured design. For example : While refactoring some of old code, I realized that by applying bridge pattern number of classes can be transformed from x*y => x+y. Same can happen if you think of decorator pattern.
So as I said, you need to understand if this 20 is because of x*y or x+y.

A: It happens that I need more than three classes for MVC - if the controller has to do something that is really complex, and it's better to extract the complexity in a separate class, rather than making the controller bigger and bigger. Or if the view has a complex sub view, especially if that subview can be reused elsewhere.
That said, any extra class is extra complexity. So removing a small amount of complexity into a separate class is usually bad. If three classes have turned into 20, then unless what your controller was supposed to do was extraordinarily complex, this may have happened here.

redpajama_set_name: RedPajamaStackExchange


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Our attorneys are graduates of the most prestigious universities and law schools in the nation, bringing a diverse background and wealth of experience in providing transactional, litigation and regulatory guidance. Marquee Law Group, APC emphasizes excellence and commitment to caring for our clients' needs which has enabled us to foster successful long-term relationships with clients and respect in the legal field.
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Poya Ghasri, Marquee Law Group, APC's Co-Founder, has focused his energy on overseeing the firm's civil litigation practice, whereby our attorneys litigate complex business, real estate, entertainment, commercial, and employment law matters. Since receiving his Juris Doctorate from the UCLA School of Law, Mr. Ghasri has dedicated his career to protecting his client's interests and supporting their intricate needs. Through his leadership, Marquee Law Group, APC, has successfully litigated numerous matters spanning multiple industries, obtaining phenomenal results for our clients. He has substantial experience handling multifaceted real estate, breach of fiduciary duty, breach of contract, business torts and employment law matters.
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Serving as Of-Counsel to Marquee Law Group, APC, Mark Bookman brings a unique blend of hands-on management experiences and in-depth knowledge of the law and public policy for tax-exempt organizations to our clients. Mr. Bookman has represented the interests of non-profit organizations for over three decades through multiple positions, whereby he acted as an officer, director, senior executive, in-house counsel and/or consultant. He received his B.A. in 1970 from the University of California at Los Angeles in History and his Juris Doctorate from the UCLA School of Law in 1973. Since 1973, he has been a good standing member of the California Bar Association.
Before joining Marquee, Mr. Bookman served as the Provost and Senior Vice-President for the American Jewish University (AJU). Prior to his time at the AJU, Mr. Bookman served as the Assistant Vice President of Student Affairs at the University of Houston and the General Manager of Associated Students at California State University, Chico. In these positions, Mr. Bookman demonstrated his strength in taking struggling organizations and transforming them into service oriented and financially successful entities. He has also served numerous professional associations, including membership on the Executive Committee of the Association of College Unions – International and as President of The Auxiliary Organization Associations of the California State Universities. As an administrator, Mr. Bookman has made numerous presentations to both regional and national associations on taxation and unfair competition issues, privatization of services, resource maximization, systems development and other related topics.
Today, Mr. Bookman works hand-in-hand with executives from various non-profit organizations, associations, and foundations, preparing their governing documents, providing guidance to their board of directors, consulting on mergers and acquisitions, and evaluating the restructuring and financing obligations for operations. He brings forth his experiences as a senior executive in a private institution, coupled with his extensive legal training, to support our clients in their philanthropic and community initiative endeavors.
Gary S. Brotman
Gary S. Brotman serves as the Senior Associate and head of the MLG Advocacy Group at Marquee Law Group, APC, whereby the firm works diligently in advocating for clients in consumer litigation matters. Mr. Brotman currently specializes in representing clients in complex employment and personal injury matters. Mr. Brotman received his Juris Doctorate from Drexel University and is a good standing member of the California Bar.
Prior to joining Marquee, Mr. Brotman served as a Deputy City Attorney for the Los Angeles City Attorney's Office, where he successfully prosecuted numerous cases on behalf of the State of California. During his time at the City Attorney's office, Mr. Brotman devoted his time to serving our community and litigating cases on behalf of the state in an effort to keep our community safe. From the onset, Mr. Brotman proved his commitment to the law and passion as a litigator.
Mr. Brotman represents plaintiffs in all areas of civil ligation including catastrophic personal injury, wrongful death, premises liability and insurance bad faith. He has dedicated his time fighting aggressively for the under-served for years. Mr. Brotman is an accomplished negotiator and zealous advocate for his clients, and is always eager to go the extra mile.
Edwin Hermawan
Edwin Hermawan is an Associate in Marquee Law Group, APC, Technology Transactions Division, focusing his efforts on representing clients in various start-ups in media, technology, and venture capital. Upon receiving his Juris Doctorate from the UCLA School of Law, Mr. Hermawan became a good standing and licensed member of the bar in New York and California. Prior to joining Marquee Law Group, APC, he began his career at the prestigious law firm of Kramer Levin & Frankel, LLP in New York.
Mr. Hermawan dedicates his practice to serving both national and international clients, working diligently on matters domestically and in Asia. He consults and provides guidance to executives regarding mergers and acquisitions, financing, capital infusions, compensation packages, and licensing agreements.
During his free time, Mr. Hermawan has successfully launched multiple technology and software companies from the ground up. This began as his creative passion, but subsequently, he was able to direct his passion, experiences, and training to serve the needs of our clients.
Anna Cai
Anna Cai is an Associate at Marquee Law Group, APC. Ms. Cai received her B.A. in History from UC Berkeley, her Juris Doctorate from the prestigious UCLA School of Law, and is a member in good standing with the California State Bar.
Prior to joining Marquee, Ms. Cai worked at public defender offices in Los Angeles, San Diego, and Contra Costa County. Ms. Cai has worked extensively with clients through every phase of their trials in multiple counties. Ms. Cai has also worked in courthouse self-help centers assisting self-represented litigants.
Ms. Cai works with Marquee's transactional and litigation practices and zealously advocates for all of her clients. Ms. Cai has been actively working on litigation matters in employment law and business law, as well as public works compliance matters for alternative energy companies. Ms. Cai's passion and determination led her to become a strategic, hard-working and assertive attorney working to serve her clients.


Handel was one of the greatest Baroque-era composers and famous for his operas, oratorios, and cantatas.
Born in Halle to a barber-surgeon who wished him to study law (which he started), Handel showed musical talent at age 7, and was encouraged by his mother to study music with a local church organist. After his father's death in 1703 he became a professional organist for churches in Halle and Hamburg. After time working in Italy he became Kapellmeister to George, Elector of Hanover. When George became George I of Great Britain, Handel moved to London in 1710, where he lived for the remainder of his life.
Handel is known for his prodigious output: he has written 42 operas (including Serse, Orlando, Agrippina, Giulio Cesare, and Rodelinda), 29 oratorios (including Saul, Israel in Egypt, Sampson, Judas Maccabaeus, and Messiah), over 120 cantatas (including Ode to St. Cecilia's Day, Acis and Galatea, and Semele), numerous trios and duets, chamber pieces, religious anthems and works (including the "Dettingen" Te Deum), and sixteen organ concerti.


Josephine C. Adams, age 74, of Broxton, Georgia passed away on Monday October 15, 2018 at Coffee Regional Medical Center. Mrs. Adams was born on February 26, 1944 in Coffee County, Georgia the daughter of the late Leland Carter and Eudine Sellers Carter.
She worked with the Coffee County School System as a custodian for over 33 years and was member of Broxton Baptist Church.
Mrs. Adams was preceded in death by a son, Kenny Myers, daughter-in-law, Debbie Myers and granddaughter, Christine Myers.
Survivors include her husband, Buddy Adams of Broxton, GA; daughter, Gina Marie Myers of Broxton, GA; two grandchildren, Jeremy Myers (wife Mary) of Broxton, GA and Jamie Myers of Broxton, GA; three great grandchildren, Jerri Lynn Lindsey (husband David), Chelsea Wolfe and Ainsley Myers; two great great grandsons, Hunter Myers and Case Lindsey; several nieces and nephews.
Funeral services will be held Wednesday October 17, 2018 at 2:00pm at Broxton Baptist Church with Rev. Milton Pate officiating. Mrs. Adams will lay-in-state Wednesday from 1 until 2pm at the church. Interment will follow at Broxton City Cemetery. The family will receive friends Tuesday evening from 6 until 9:00pm at Sims Funeral Home.
Sympathy may be expressed by signing the online registry at www.simsfuneralhome.com.
Sims Funeral Home in charge of arrangements.


Naming babies vs. naming your business - How to choose a business name.
First of all, with baby names there are only two people who have a say in the decision. It's a simple democratic process where the wife always has veto power over anything the husband comes up with.
With company names, you have to get the consensus of many people. Sometimes there are even committees involved, which usually lead to winning names like Poolife for a swimming pool cleaning company.
Doesn't work that way in the business world. There are hordes of lawyers who do nothing but trademark protection and application work. So if your product name even sounds like something that's already out there, you're in trouble. Case in point: There was a little coffee shop in the small town of Astoria, Oregon that got sued by Starbucks for trademark infringement. It was called Sambucks.
And then there's the whole translation issue. Face it, you probably don't care what "Clark" means in Hungarian. But there are dozens of stories of product names like the Chevy Nova, which didn't translate real well. (In Spanish, Nova means "does not go.") If you're doing business globally, your naming project just got astronomically harder.
And here's an important distinction: your child's livelihood doesn't depend on people remembering his or her name. Sure, unfortunate names like Major Slaughter, Ima Nut or Moon Unit might cause a lifetime of grief, but they won't make or break the poor kid's career like a bad product name can.
• Totally boring, literal names like the now defunct Third Street Coffee House.
• Names that backfire completely when applied to internet URLs. Need a therapist? Try www.therapistfinder.com. Need some good art, go to www.speedofart.com. Looking for a nice pen? www.penisland.com.
A good name can be costly, but not nearly as costly as blunders like that. So save yourself a lot of time, money and frustration and just hire a branding firm to help from the very beginning. Not a design firm… they focus on the language of images, not words. And not an ad agency… For some reason, ad agencies love to use one-word names that are just too cool for school. Like "North" "Red F" "Citrus" "Fuel" If you want to confuse people, just follow that lead.
• Dress Barn??? How many women will admit to shopping there, much less bringing herds friends in? Tough to be a brand ambassador for a place called the Dress Barn.
Your name is the foundation of your brand. So if your business IS your baby, get started right with a memorable name. Call BNBranding for affordable help with your brand name and identity.


text:
\section{Introduction}

Neutral atomic hydrogen (H{\sc i}) and molecular hydrogen (${\rm H_2}$) are the key components of the cold interstellar medium (ISM) in galaxies, and are the fuel for star formation. The distribution of baryons between atomic gas, molecular gas, and stars is an important indicator of the evolutionary stage of a galaxy: at early times, most of the baryonic mass is in the atomic phase, while, for highly evolved systems (e.g. red and dead ellipticals), almost all the baryons are in the stars. The relative contributions of atomic gas, molecular gas, and stars to the total baryonic mass in galaxies, and the evolution of these contributions over cosmological time are thus critical inputs to studies of galaxy evolution. In the local Universe, most of the baryonic content in massive star-forming galaxies at $z\approx0$ is in stars, while H{\sc i}\ makes up $\approx 70-90$\% of the cold-gas content of most such galaxies \citep[e.g.][]{Saintonge17,Catinella18}.

At high redshifts, CO observations of star-forming galaxies at $z \approx 1 - 3$ have found evidence for large reservoirs of molecular gas, comparable in mass to their stellar masses  \citep[e.g.][]{Daddi10,Tacconi13,Tacconi18}. This is very different from the situation in galaxies at $z \approx 0$, where the ratio of the molecular gas mass to the stellar mass is only $\approx 0.02-0.10$ \citep{Saintonge17}. Indeed, the molecular gas mass of main-sequence galaxies has been observed to increase by approximately an order of magnitude from $z\approx0$ to $z\approx2$ \citep[e.g.][]{Genzel15,Tacconi20}. The large inferred molecular gas content of high-$z$ galaxies has been used to argue that the cold-gas content of galaxies at $z\approx1-3$ is predominantly of molecular form \citep[e.g.][]{Tacconi18}.

Measurements of the atomic and molecular content of high-$z$ galaxies provide important constraints on numerical and semi-analytical models of galaxy evolution  \citep[e.g.][]{Obreschkow09,Lagos11,Popping14,Dave19,Dave20}. Unfortunately, the weakness of the H{\sc i} 21\,cm\ line, the only tracer of the H{\sc i}\ content of galaxies, has made it very challenging to directly measure the H{\sc i}\ mass of galaxies at cosmological distances. Indeed, even at intermediate redshifts, there are only a handful of galaxies at $z\approx0.2-0.4$ for which estimates of $\rm{M_{Atom}}/\rm{M_{Mol}}$ are available \citep{Cybulski16,Fernandez16,Cortese17}. As a result, it has hitherto not been possible to  measure the redshift evolution of $\rm{M_{Atom}}/\rm{M_{Mol}}$ and directly test the hypothesis that most of the cold gas in star-forming galaxies at $z \approx 1-3$ is in the molecular phase.

Recently, the H{\sc i} 21\,cm\ stacking approach has been  used to measure the {\it average} H{\sc i}\ mass of star-forming galaxies out to $z\approx1.3$ \citep{Bera19,Chowdhury20,Chowdhury21}. \citet{Chowdhury20} used the upgraded Giant Metrewave Radio Telescope (GMRT) to measure, for the first time, the average H{\sc i}\ mass of galaxies at $z\approx1$, by stacking the H{\sc i} 21\,cm\ emission signals of 7,653 blue star-forming galaxies at $z=0.74-1.45$ in the DEEP2 survey fields \citep{Newman13}. More recently,  \citet[][hereafter, \citetalias{Chowdhury22a}]{Chowdhury22a}  used the GMRT Cold-H{\sc i}\ AT $z\approx1$ (CAT$z1$) survey (\citealp{Chowdhury22b}; hereafter, \citetalias{Chowdhury22b}), a 510-hr upgraded GMRT H{\sc i} 21\,cm\ emission survey of galaxies at $z=0.74-1.45$, also in the DEEP2 survey fields, to measure the average H{\sc i}\ mass of star-forming galaxies in two stellar-mass-matched subsamples at $z=0.74-1.25$ and $z=1.25-1.45$. \citetalias{Chowdhury22a} found that the average H{\sc i}\ mass of main-sequence galaxies declines steeply from $z\approx1.3$ to $z\approx1.0$, by a factor of $3.2\pm0.8$.

In this \emph{Letter}, we combine the GMRT-CAT$z1$ measurements of the average H{\sc i}\ mass of star-forming galaxies at $z\gtrsim1$ with estimates of the average ${\rm H_2}$\ mass and the average stellar mass of the same galaxies, to estimate, for the first time, the contribution of atomic gas, molecular gas, and stars to the baryonic mass of galaxies at $z \gtrsim 1$, nearly nine billion years ago.

{Throughout this \emph{Letter}, we use a flat Lambda-cold dark matter cosmology, with $\Omega_m=0.3$, $\Omega_\Lambda = 0.7$, and $H_0 = 70$~km~s$^{-1}$~Mpc$^{-1}$. All estimates of stellar masses and SFRs assume a Chabrier initial mass function (IMF); stellar masses and SFRs from the literature that assume a Salpeter IMF were converted to a Chabrier IMF by subtracting 0.2~dex \citep[e.g.][]{Madau14}. }

\section{The cold gas content of galaxies at $z \approx 1$ and in the local Universe}
\label{sec:analysis}

\subsection{Atomic Gas in Star-forming Galaxies at $z=0.74-1.45$}
\begin{figure}
    \centering
    \includegraphics[width=\linewidth]{Figure1.pdf}
    \caption{The stellar mass distribution of the galaxies in the three redshift intervals. Panel~(A) shows the stellar mass distribution of the blue galaxies of the xGASS sample \citep[blue histogram;][]{Catinella18} and those of the xCOLD~GASS sample \citep[green histogram;][]{Saintonge17}. Panels~(B) and (C) show the stellar-mass distributions of the GMRT-CAT$z1$ subsamples at $z=0.74-1.25$ and $z=1.25-1.45$ \citepalias[blue histograms;][]{Chowdhury22a}. All average quantities reported in this work, for the three subsamples at $z\approx0$, $z\approx1.0$, and $z\approx1.3$, were computed with weights such that the  stellar-mass distribution of each subsample is identical to that of the subsample at $z=1.25-1.45$ (the orange histogram in each panel). The number of galaxies in each subsample is listed in each panel. }
    \label{fig:stellar-mass}
\end{figure}
\begin{figure}
    \centering
    \includegraphics[width=\linewidth]{Figure2.pdf}
    \caption{The stacked H{\sc i} 21\,cm\ spectra of blue star-forming galaxies at $z=0.74-1.25$ (left panel) and $z=1.25-1.45$ (right panel) from \citetalias{Chowdhury22b}. The stacked H{\sc i} 21\,cm\ spectrum of each panel was obtained by stacking the individual H{\sc i} 21\,cm\ spectra of the galaxies in the subsample, using weights to ensure that the stellar-mass distributions of the two subsamples are identical. The dashed curve in each panel shows the $1\sigma$ RMS noise error on each 90~km~s$^{-1}$\ velocity channel of the stacked H{\sc i} 21\,cm\ spectrum. }
    \label{fig:HIstacks}
\end{figure}

The GMRT-CAT$z1$ survey provides measurements of the average H{\sc i}\ mass of star-forming galaxies in two stellar-mass matched subsamples at $z=0.74-1.25$ and $z=1.25-1.45$  \citepalias{Chowdhury22a}. The H{\sc i} 21\,cm\ stacking analysis used to obtain the average H{\sc i}\ mass estimates is described in detail in \citetalias{Chowdhury22a}. We provide here a summary of relevant information on the sample of galaxies, and the H{\sc i} 21\,cm\ stacking analysis and results, for the two redshift intervals.

The main sample of the GMRT-CAT$z1$ survey contains 11,419 blue star-forming galaxies with $\textrm{M}_*\geq10^{9}~\textrm{M}_\odot$ at $z=0.74-1.45$ in seven GMRT pointings on the DEEP2 survey fields \citepalias{Chowdhury22b}.  The stellar masses of the 11,419 galaxies were inferred from their rest-frame U$-$B colours, rest-frame B$-$V colours and rest-frame absolute B-band magnitudes  \citep{Weiner09}; the relation was calibrated via comparisons with DEEP2 galaxies at similar redshifts in regions with K-band photometry \citep{Weiner09}. {The SFRs of the 11,419 galaxies of our sample were inferred using a calibration from \citet{Mostek12}, based on their rest-frame B-band magnitudes and the rest-frame (U-B) colours.\footnote{This SFR calibration was derived by \citet{Mostek12} for DEEP2 galaxies in the Extended Groth Strip for which SFRs were obtained by \citet{Salim09} via spectral-energy distribution (SED) fits to the ultraviolet, optical, and near-infrared photometry. \citet{Salim09} found the SFRs inferred from the SED fits to be consistent with the mid-infrared luminosities of the DEEP2 galaxies.}} Dividing the galaxies into multiple redshift and stellar-mass bins, the average stellar masses and the average SFRs of galaxies in each bin are found to be consistent with the star-forming main sequence \citep{Whitaker14} at these redshifts \citepalias{Chowdhury22a}.

The GMRT-CAT$z1$ survey provides H{\sc i} 21\,cm\ subcubes for the 11,419 galaxies at a spatial resolution of 90~kpc and a velocity resolution of 90~km~s$^{-1}$\ \citepalias{Chowdhury22b}. {The subcubes of each galaxy were converted from flux density} ($\rm{S_{H{\textsc i}}}$, { in units of Jy) to luminosity density } ($\rm{L_{H{\textsc i}}}$, { in units of  Jy~Mpc$^2$) using the relation} $\rm{L_{H{\textsc i}} =4\pi~S_{H{\textsc i}}~D_L^2/(1+z)}$, { where ${\rm d_L}$ is the luminosity distance of the galaxy, in Mpc.} The spatial resolution of 90~kpc was chosen to ensure that the average H{\sc i} 21\,cm\ emission from the full sample of 11,419 galaxies is spatially unresolved \citepalias{Chowdhury22b}.

The measurement of the average H{\sc i}\ mass of galaxies in the two redshift bins was obtained by dividing the 11,419 galaxies into two redshift subsamples, with $z=0.74-1.25$ (9284 galaxies) and $z=1.25-1.45$ (2135 galaxies), and separately stacking the H{\sc i} 21\,cm\ subcubes of the galaxies in each subsample \citepalias{Chowdhury22a}. The effective stellar-mass distributions of the two redshift subsamples were made identical by applying weights to the galaxies of the lower-$z$ sample during the stacking procedure; { the stellar-mass distributions of the two redshift subsamples are shown in Fig.~\ref{fig:stellar-mass}.} The average stellar mass of the subsample at $z\approx1.3$ is $\approx10^{10}~\textrm{M}_\odot$. The stacked H{\sc i} 21\,cm\ spectral cube of each subsample of galaxies was then obtained by using the above weights to take a weighted average of the H{\sc i} 21\,cm\ subcubes of the DEEP2 galaxies in each subsample. { The RMS noise on each of the stacked H{\sc i} 21\,cm\ spectral cubes was estimated using Monte Carlo simulations, taking into account the stellar-mass based weights of the galaxies in each subsample \citepalias{Chowdhury22a}.} We note that the final stacked GMRT H{\sc i} 21\,cm\ spectral cubes have a spatial resolution of 90~kpc. The compact GMRT beam ensures that the measurements of the average H{\sc i}\ mass of galaxies in the GMRT-CAT$z1$ survey are not significantly affected by H{\sc i} 21\,cm\ emission from companion galaxies around the target galaxies, i.e. by source confusion \citepalias{Chowdhury22b}.

The average H{\sc i}\ masses of the galaxies in the two redshift subsamples were derived from their stacked H{\sc i} 21\,cm\ subcubes using the following procedure: (i)~the central velocity channels of the stacked cube were averaged to obtain a stacked H{\sc i} 21\,cm\ emission image of the subsample, (ii)~the H{\sc i} 21\,cm\ spectrum at the location of the peak luminosity-density in the stacked H{\sc i} 21\,cm\ emission image was extracted, (iii)~contiguous central velocity channels of the stacked spectrum, with emission detected at $> 1.5\sigma$ statistical significance, were integrated to measure the average velocity-integrated H{\sc i} 21\,cm\ line luminosity ($\int \rm{L_{H{\textsc i}} \ dV}$, in units of ${\rm Jy~Mpc^2}$~km~s$^{-1}$) of the subsample, and (iv)~the average velocity-integrated line luminosity was converted to the average H{\sc i}\ mass of the subsample via the relation  $\rm{M_{H{\textsc i}}}=[1.86 \times 10^4 \times \int \rm{L_{H{\textsc i}} \ dV}]~\textrm{M}_\odot$.

The stacked H{\sc i} 21\,cm\ emission spectra of the 9284 galaxies at $z = 0.74-1.25$ and the 2135 galaxies at $z=1.25-1.45$ are shown in Fig.~\ref{fig:HIstacks}. For both redshift subsamples, the stacked H{\sc i} 21\,cm\ emission signal is clearly detected, at $>5.2~\sigma$ statistical significance. { We convert the measured average H{\sc i}\ mass of galaxies in each subsample to an estimate of the average atomic gas mass of the subsample using the relation} $\langle\rm{M_{Atom}}\rangle=1.36 \times \langle \rm{M_{H{\textsc i}}} \rangle$, { where the factor of 1.36 accounts for the mass contribution of helium.}  The average atomic gas masses of the galaxies in the two subsamples are listed in Table~\ref{tab:mass}.

\subsection{Atomic Gas in Star-forming Galaxies at $z\approx0$}
We use the extended GALEX Arecibo SDSS Survey \citep[xGASS;][]{Catinella18} of nearby galaxies as a reference sample, to compare the H{\sc i}\ properties of galaxies at $z\gtrsim1$ to those of galaxies in the local Universe. xGASS is an H{\sc i} 21\,cm\ survey of a stellar-mass selected sample of local-Universe galaxies with $\textrm{M}_*>10^{9} \ \textrm{M}_\odot$ \citep{Catinella18}. Each galaxy in the xGASS sample was observed with the Arecibo Telescope until either a detection of the H{\sc i} 21\,cm\ emission was obtained or a $3\sigma$ upper limit of $\leq 0.1$ was achieved on the ratio of the H{\sc i}\ mass to the stellar mass. In order to carry out a fair comparison with our sample of blue star-forming galaxies at $z\approx1$, we used only the 569 blue xGASS galaxies, with $\rm NUV - r < 4$, as the reference sample. The stellar masses of all the xGASS galaxies are available from the Sloan Digital Sky Survey DR7 MPA-JHU catalog \citep{Kauffmann03,Brinchmann04}; { Figure~\ref{fig:stellar-mass}[A] shows the stellar mass distribution of the 569 blue xGASS galaxies.}

We measured the average H{\sc i}\ mass of the blue xGASS galaxies, using weights such that the stellar-mass distribution of the blue xGASS sample is identical to that of our DEEP2 galaxies at $z=1.25-1.45$.  {  The H{\sc i} 21\,cm\ line was not detected for 16 of the 569 blue galaxies; for these 16 galaxies, we assume that the H{\sc i}\ mass is equal to the $3\sigma$ upper limit on} $\rm{M_{H{\textsc i}}}$. { The error on the average H{\sc i}\ mass was estimated using bootstrap resampling with replacement. We note that we used the same stellar-mass based weights during the bootstrap resampling procedure in order to compute the weighted-average H{\sc i}\ mass of each randomly-drawn subsample. Finally, we again converted the average H{\sc i}\ mass of the sample to the average atomic gas mass via the relation} $\langle\rm{M_{Atom}}\rangle=1.36 \times \langle\rm{M_{H{\textsc i}}}\rangle$.  Table~\ref{tab:mass} lists the average atomic gas mass of the blue xGASS galaxies at $z\approx 0$, with $\langle \textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$.

\subsection{Molecular Gas in Star-forming Galaxies at $z=0.74-1.45$}

The H$_2$ mass of galaxies is typically estimated from tracers of molecular gas, such as the CO rotational lines, the far-infrared dust continuum, or the 1-mm dust continuum \citep[e.g.][]{Tacconi20}, with the different methods based on different assumptions and calibration schemes.
 \citet{Tacconi20} used a compilation of molecular gas mass estimates from the literature (including the mass contribution from helium) to provide the following relation between the molecular gas depletion timescale ($\rm t_{dep;mol}=M_{Mol}$/SFR) of galaxies and their (i)~redshift, (ii)~stellar mass, and (iii)~offset from the star-forming main-sequence at the galaxy redshift:

\begin{equation}
    \log[{\rm t_{dep;mol}/Gyr}] = {\rm A} - {\rm B} \times \log[1 + z] + {\rm C} \times \log[{\rm sSFR}/{\rm sSFR}({\rm MS}, z, \textrm{M}_* )] + {\rm D} \times (\log[\textrm{M}_*/\textrm{M}_\odot] - 10.7)\ \ ,
    \label{eqn:tacconi20}
\end{equation}

\noindent where sSFR ($\rm \equiv SFR/\textrm{M}_*$) is the specific star-formation rate, ${\rm sSFR}({\rm MS}, z, \textrm{M}_* )$ is the sSFR of galaxies with stellar mass $\textrm{M}_*$  lying on the star-forming main-sequence at redshift $z$, and the values of the co-coefficients are A$=0.21\pm0.10$, B$=-0.98\pm0.10$, C$=-0.49\pm0.03$, and D$=0.03\pm0.04$ \citep[where the quoted errors are $2\sigma$ uncertainties; ][]{Tacconi20}. The relation was obtained from a sample of $2052$ galaxies with redshifts $z \approx 0 - 5.3$, stellar masses $\textrm{M}_* \approx 10^9 - 10^{12.2} \ \textrm{M}_\odot$, and SFRs~$\approx 0.04 - 5600 \ \textrm{M}_\odot$~yr$^{-1}$ \citep{Tacconi20}.

We use Equation~\ref{eqn:tacconi20} to estimate the molecular  gas depletion timescale of each of the 11,419 GMRT-CAT$z1$ galaxies. Next, we combine the molecular depletion timescales of the individual galaxies with their SFRs to infer the molecular gas  mass of each galaxy. Finally, we take a weighted mean of the $\rm{M_{Mol}}$ values in the two redshift subsamples, with the same weights (see Fig.~\ref{fig:stellar-mass}) that were used while stacking the H{\sc i} 21\,cm\ emission from each subsample.
The estimated average molecular gas masses of the galaxies in the two redshift subsamples are listed in Table~\ref{tab:mass}.

{ The errors on the coefficients A, B, C, and D were propagated via a Monte Carlo approach to estimate the formal error on the average molecular gas mass of each subsample, appropriately taking into account the weight associated with each galaxy in the subsample}; these errors are listed in Table~\ref{tab:mass}.  \citet{Tacconi20} note that systematic uncertainties in reduced quantities like the sSFR have little effect on the inferred ${\rm t_{dep;mol}}$. This is even more the case for our sample of DEEP2 galaxies, which lie on the main sequence \citepalias{Chowdhury22a}; we have further verified that even excluding the sSFR dependence from Equation~\ref{eqn:tacconi20} has no significant effect on the average molecular gas mass.
However, we note that the formal error on the average molecular gas mass for each subsample does not include uncertainties stemming from the assumptions (e.g. the CO-to-H$_2$ conversion factor, $\alpha_{\rm CO}$) made in the molecular gas mass estimates of the original sample of 2052 galaxies. \citet{Tacconi20} estimate that the uncertainty arising from the assumptions is $\approx 0.25$~dex; the effect of these uncertainties is discussed in Section~\ref{sec:discuss}.

Although Equation~\ref{eqn:tacconi20} was obtained from a sample of galaxies with $\textrm{M}_* \approx 10^9 - 10^{12.2} \ \textrm{M}_\odot$ and at $z \approx 0-5.3$, the vast majority of $\rm{M_{Mol}}$ estimates in galaxies at $z \gtrsim 0.5$ are for objects with $\textrm{M}_* \gtrsim 10^{10} \ \textrm{M}_\odot$ \citep[e.g.][]{Tacconi20}. The stellar mass of the DEEP2 galaxies in the GMRT CAT$z$1 survey extends down to $10^9 \ \textrm{M}_\odot$ at $z \approx 0.74 - 1.45$ \citepalias{Chowdhury22a}, implying that we are applying the relation of \citet{Tacconi20} in a regime where it is not well constrained.

However, an alternative way to estimate the molecular gas masses of the DEEP2 galaxies is from the molecular gas depletion timescale, which is $\approx 0.7$~Gyr in main-sequence galaxies at $z\approx1$, with only a weak dependence on the stellar mass \citep{Tacconi13,Genzel15}. Assuming a constant molecular gas depletion timescale of $0.7$~Gyr, we find that the inferred average $\rm{M_{Mol}}$ values for the GMRT-CAT$z1$ galaxies are consistent with those obtained from Equation~\ref{eqn:tacconi20}. It is hence unlikely that our estimates of the average $\rm{M_{Mol}}$ of star-forming galaxies at $z\approx1.0$ and $z\approx1.3$ are significantly affected by the above extrapolation to lower stellar masses.

\begin{table}[]
    \centering
    \begin{tabular}{|l|c|c|c|}
        \hline\hline
         & $z\approx0$ & $z\approx1$ & $z\approx1.3$  \\
         \hline
       Average Stellar Mass, $\langle\textrm{M}_*\rangle$ ($10^9~\textrm{M}_\odot$) & $10.3 \pm 2.4$ & $10.3 \pm 2.4$ & $10.3 \pm 2.4$  \\
       Average Atomic Gas Mass, $\langle \rm{M_{Atom}} \rangle$ ($10^9~\textrm{M}_\odot$) & $5.59\pm0.24$ & $14.4\pm2.6$ & $45.7\pm8.7$ \\
      Average Molecular Gas Mass, $\langle \rm{M_{Mol}} \rangle$ ($10^9~\textrm{M}_\odot$) & $0.974\pm0.048$ & $6.22\pm0.78$ & $9.19\pm1.17$ \\
     Average Baryonic Mass, $\langle \textrm{M}_\textrm{Baryon} \rangle$ ($10^9~\textrm{M}_\odot$) & $16.86\pm2.4$ & $30.9\pm3.6$ & $65.3\pm9.1$ \\
        \hline
        \hline
    \end{tabular}

    \caption{The average masses of the key baryonic constituents of stellar-mass matched samples of blue star-forming galaxies at three different redshifts, $z \approx 0$, $z \approx 1$, and $z \approx 1.3$. The four rows list, for each redshift, (1)~the average stellar mass, $\langle\textrm{M}_*\rangle$, (2)~the average atomic gas mass, $\langle\rm{M_{Atom}}\rangle$, including the mass contribution from helium, (3)~the average molecular gas mass, $\langle\rm{M_{Mol}}\rangle$, again including the mass contribution from helium, and (4)~the total average baryonic mass,  $\langle\rm{M_{Baryon}}\rangle\equiv\langle\textrm{M}_*\rangle+\langle\rm{M_{Atom}}\rangle+\langle\rm{M_{Mol}}\rangle$.
    The average atomic gas masses of blue star-forming galaxies at $z\approx1.0$ and $z\approx1.3$ are from the GMRT-CAT$z1$ survey \citepalias{Chowdhury22a}, with the average molecular gas masses of the same galaxies estimated using Equation~\ref{eqn:tacconi20} \citep{Tacconi20}. The average atomic gas and molecular gas masses of blue star-forming galaxies at $z\approx0$ were obtained, respectively, from the xGASS and xCOLD~GASS surveys \citep{Saintonge17,Catinella18}.  The errors indicate the $1\sigma$ uncertainties in the estimates. See text for discussion.}
    \label{tab:mass}
    \end{table}

\begin{table}[]
\centering
\begin{tabular}{|l|c|c|c|}
\hline\hline
    & $z\approx0$ & $z\approx1$ & $z\approx1.3$  \\
    \hline
    & & & \\
    Average atomic-gas-to-stars mass ratio,    $\langle \rm{M_{Atom}} \rangle$/$\langle\textrm{M}_*\rangle$ & $0.54^{+0.17}_{-0.10}$ & $1.40^{+0.51}_{-0.35}$ & $4.44^{+1.65}_{-1.14}$ \\[0.15cm]
    Average molecular-gas-to-stars mass ratio,     $\langle \rm{M_{Mol}} \rangle$/$\langle\textrm{M}_*\rangle$  & $0.095^{+0.029}_{-0.018}$ & $0.60^{+0.20}_{-0.13}$ & $0.89^{+0.30}_{-0.20}$ \\[0.25cm]
       \hline
       & & &\\
    Average atomic-gas-to-baryons mass ratio,   $\langle \rm{M_{Atom}} \rangle$/$\langle \textrm{M}_\textrm{Baryon} \rangle$ $\times10^2$ & $33.1^{+5.6}_{-4.2}$ & $46.6^{+5.8}_{-6.0}$ & $70.1^{+4.6}_{-5.4}$ \\[0.15cm]
     Average molecular-gas-to-baryons mass ratio,   $\langle \rm{M_{Mol}} \rangle$/$\langle \textrm{M}_\textrm{Baryon} \rangle$ $\times10^2$ & $5.78^{+1.01}_{-0.77}$ & $20.1^{+3.3}_{-2.9}$ & $14.1^{+2.8}_{-2.3}$ \\[0.15cm]
     Average stars-to-baryons mass ratio,    $\langle\textrm{M}_*\rangle$/$\langle \textrm{M}_\textrm{Baryon} \rangle$ $\times10^2$ & $61.1^{+6.5}_{-4.9}$ & $33.3^{+6.1}_{-5.8}$ & $15.8^{+3.6}_{-4.0}$ \\[0.25cm]
         \hline
         & & &\\
     Average atomic-to-molecular gas mass ratio,    $\langle \rm{M_{Atom}} \rangle$/$\langle \rm{M_{Mol}} \rangle$  & $5.74^{+0.39}_{-0.37}$ & $2.32^{+0.54}_{-0.47}$ & $5.0^{+1.2}_{-1.0}$ \\[0.25cm]
        \hline
        \hline
    \end{tabular}
    \caption{The ratios of the average masses of the key baryonic constituents of blue star-forming galaxies at three different redshifts, $z \approx 0$, $z \approx 1$, and $z \approx 1.3$. The first two rows list the ratios of the average atomic gas mass and the average molecular gas mass to the average stellar mass. The next three rows list the ratios of the average atomic gas mass, the average molecular gas mass, and the average stellar mass to the average total baryonic mass. Finally, the last row lists the ratio of the average atomic gas mass to the average molecular gas mass.  The errors indicate the $1\sigma$ uncertainties in the estimates. See text for discussion. }
    \label{tab:ratios}
\end{table}

\subsection{Molecular Gas in Star-forming Galaxies at $z\approx0$}

  We use the extended CO Legacy Database for GASS \citep[xCOLD~GASS][]{Saintonge17} survey to compute the average molecular gas mass of a reference sample of blue star-forming galaxies at $z\approx0$. The xCOLD~GASS survey used the IRAM~30m telescope to carry out CO(1--0) observations of a sample of 532 galaxies at $z \approx 0.01-0.05$ and with stellar masses $\textrm{M}_* > 10^9 \ \textrm{M}_\odot$ \citep{Saintonge17}. Approximately $90$\% of the xCOLD~GASS galaxies are covered in the H{\sc i} 21\,cm\ line with the xGASS survey \citep{Saintonge17,Catinella18}, while stellar masses for all xCOLD~GASS galaxies are again available from the MPA-JHU catalog. To carry out a fair comparison with our high-$z$ blue star-forming galaxies, we restricted to the 287 blue xCOLD~GASS galaxies, with NUV$-$r$<4$; { the stellar mass distribution of the 287 galaxies is shown in Figure~\ref{fig:stellar-mass}[A]}. 252 of these galaxies have CO(1--0) detections, while 35 galaxies have upper limits on the CO(1--0) line luminosity \citep{Saintonge17}.
  The xCOLD~GASS catalogue provides the molecular gas mass of the galaxies, including the mass contribution from helium. We computed the average molecular gas mass of these 287 galaxies, using weights in the average such that the stellar-mass distribution of the xCOLD~GASS galaxies is identical to that in Fig.~\ref{fig:stellar-mass}[C], i.e. identical to that of the GMRT-CAT$z1$ galaxies at $z=1.25-1.45$. For the 35~galaxies with CO(1--0) non-detections, we assume that the molecular gas mass is equal to the $3\sigma$ upper limit on $\rm{M_{Mol}}$, provided by the xCOLD~GASS survey. The average molecular gas mass thus obtained is listed in Table~\ref{tab:mass}; {the error on this quantity was obtained from bootstrap resampling with replacement, accounting for the stellar-mass-based weight of each galaxy. }

\section{Results and Discussion}
\label{sec:discuss}

\begin{figure*}
    \centering
    \includegraphics[width=\linewidth]{Figure3.pdf}
    \caption{The redshift evolution of (A)~the ratios of the average atomic gas mass and the average molecular gas mass to the average stellar mass, and (B)~the ratios of the average atomic gas mass, the average molecular gas mass, and the average stellar mass to the average baryonic mass. In both panels, all plotted values are for stellar-mass matched samples of galaxies with $\langle\textrm{M}_*\rangle \approx10^{10}~\textrm{M}_\odot$ at $z\approx0$, $z\approx1.0$ and $z\approx1.3$.  The error bars along the y-axis show the $1\sigma$ uncertainties in the estimates. See text for discussion.}
    \label{fig:baryonfraction}
\end{figure*}

\begin{figure*}
    \centering
    \includegraphics[width=0.65\linewidth]{Figure4.pdf}
    \caption{The ratio of the average atomic gas mass to the average molecular gas mass in stellar-mass matched samples of star-forming galaxies at $z\approx0$, $z\approx1.0$, and $z\approx1.3$. The blue circle shows the estimated value of $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Mol}} \rangle$ in star-forming galaxies at $z\approx0$ \citep{Saintonge17,Catinella18}. The red squares show estimates of $\langle\rm{M_{Atom}}\rangle/\langle\rm{M_{Mol}}\rangle$ in star-forming galaxies at two redshift intervals $z=0.74-1.25$ and $z=1.25-1.45$. The error bars along the y-axis show the $68.3\%$ confidence intervals on $\langle\rm{M_{Atom}}\rangle/\langle\rm{M_{Mol}}\rangle$. The dashed line indicates $\langle\rm{M_{Atom}}\rangle/\langle\rm{M_{Mol}}\rangle=1$. It is clear that the average atomic gas mass in star-forming galaxies is higher than the average molecular gas mass over the past 9~Gyr.  }
    \label{fig:HIH2}
\end{figure*}

Table~\ref{tab:mass} lists our measurements of the average atomic gas mass, and estimates of the average molecular gas mass, of the GMRT-CAT$z1$ galaxies at $z\approx1.0$ and $z\approx1.3$, along with measurements of the average atomic gas mass and average molecular gas mass of reference samples of blue star-forming galaxies at $z\approx0$. The weights used in the averages ensure that the $z\approx 0$, $z \approx 1$, and $z\approx 1.3$ galaxy samples all have identical stellar-mass distributions, with an average stellar mass of $\langle \textrm{M}_* \rangle = 10.3 \times 10^{9} \ \textrm{M}_\odot$. We note that the listed errors on the $\langle \rm{M_{Mol}} \rangle$ values do not include uncertainties in the assumptions (e.g., the value of $\alpha_{\rm CO}$). The uncertainty on $\langle \textrm{M}_* \rangle$ is assumed to be 0.1~dex, based on comparisons between stellar-mass estimates for the same galaxies using different methods and assumption \citep[e.g.][]{Stefanon17}. The last row of the table combines the estimates of the average atomic gas mass, average molecular gas mass, and the average stellar mass to infer the average total baryonic mass of star-forming galaxies at $z\approx0$, $z\approx1.0$, and $z\approx1.3$. The average baryonic mass,  $\langle\rm{M_{Baryon}}\rangle$, for each redshift interval was estimated using $\langle\rm{M_{Baryon}}\rangle=\langle\textrm{M}_*\rangle+\langle\rm{M_{Atom}}\rangle+\langle\rm{M_{Mol}}\rangle$.

Table~\ref{tab:ratios} lists the ratios of the average atomic gas, molecular gas, and stellar masses relative to the average stellar mass and the average baryonic mass, as well as the ratio of the average atomic gas mass to the average molecular mass. We estimated the errors on each ratio via Monte Carlo simulations in which we obtained a large number of realisations of the ratio by drawing pairs of values for the average masses in the numerator and the denominator from Gaussian distributions of the two quantities, with the same means and standard derivations as the estimates of the average masses.

It is clear from Table~\ref{tab:ratios} that the baryonic composition of star-forming galaxies shows dramatic evolution over the last $\approx 9$~Gyr, from $z \approx 1.3$ to $z = 0$.
Figure~\ref{fig:baryonfraction}(A) plots the ratios of the average atomic gas and molecular gas masses (red squares and blue circles, respectively) to the average stellar mass versus redshift.  The figure shows that that both $\langle\rm{M_{Mol}}\rangle/\langle\textrm{M}_*\rangle$ and $\langle\rm{M_{Atom}}\rangle/\langle\textrm{M}_*\rangle$ decrease by roughly an order of magnitude from $z \approx 1.3$ to $z\approx0$. However, the nature of the decline is very different in the atomic and the molecular components. The ratio  $\langle\rm{M_{Atom}}\rangle/\langle\textrm{M}_*\rangle$ drops steeply, by a factor of $\approx3.3$, in the $\approx1$~Gyr period between $z\approx1.3$ and $z\approx1.0$, and then falls gradually, by a factor of $\approx2.6$, over the $\approx7$~Gyr between $z\approx1.0$ and $z\approx0.0$. Conversely, the ratio $\langle\rm{M_{Mol}}\rangle/\langle\textrm{M}_*\rangle$ falls by a factor of only $\approx1.5$ between $z\approx1.3$ and $z\approx1.0$, but then drops by a factor of $\approx6.3$ between $z\approx1$ and $z\approx0$. The rapid decline in the atomic gas mass of galaxies between $z\approx1.3$ and $z\approx1.0$, towards the end of the epoch of galaxy assembly, indicates insufficient accretion of gas from the CGM \citepalias{Chowdhury22a}; this is the likely cause for the decline in the star-formation activity of the Universe at $z\lesssim1$. Further, it is clear from Fig.~\ref{fig:baryonfraction}(A) that the atomic gas mass is significantly higher than the stellar mass, by a factor of $\approx 4.4$, at $z \approx 1.3$, during the epoch of peak star-formation activity, $z \approx 1-3$, in the universe \citep{Madau14}.

Figure~\ref{fig:baryonfraction}(B) plots the redshift evolution of the stellar, atomic gas, and molecular gas fractions of the baryonic mass. The three main baryonic components of galaxies show very different behaviours. In the local Universe, it is clear that stars dominate the baryonic content of star-forming galaxies with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$, constituting $\approx60\%$ of the baryonic mass. However, the fraction of baryons in stars decreases with increasing redshift: stars make up only $16\%$ of the baryonic mass in such galaxies at $z\approx1.3$. Conversely, Figure~\ref{fig:baryonfraction}(B) shows that the contribution of both atomic gas and molecular gas to the total baryonic mass of star-forming galaxies with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$ is significantly higher at $z \gtrsim 1$ than in the local universe. The contribution of atomic gas to the baryonic mass increases from $\approx33\%$ at $z\approx0$ to $\approx47\%$ at $z\approx1$, and then to $\approx70\%$ at $z\approx1.3$. For the molecular component, we find that $\langle\rm{M_{Mol}}\rangle/\langle\rm{M_{Baryon}}\rangle$ increases from $\approx6\%$ at $z\approx0$ to $\approx20\%$ at $z\approx1.0$, and then flattens, with $\langle\rm{M_{Mol}}\rangle/\langle\rm{M_{Baryon}}\rangle \approx 14\%$  at $z\approx1.3$. Overall, Figure~\ref{fig:baryonfraction}(B) shows that the neutral-gas fraction of the baryonic mass of star-forming galaxies with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$ at $z\gtrsim1$ is significantly higher than at $z\approx0$. Neutral gas makes up $\approx 84$\% of the baryonic mass of star-forming galaxies at $z \approx 1.3$, with atomic gas constituting $\approx70\%$ of the baryonic mass.

Finally, the values of the ratio of the average atomic gas mass to the average molecular gas mass in star-forming galaxies with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$ at $z\approx0$, $z\approx1.0$ and $z\approx1.3$ are listed in Table~\ref{tab:mass} and plotted against redshift in Figure~\ref{fig:HIH2}. We find that $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Mol}} \rangle$ decreases from $5.74^{+0.39}_{-0.37}$ in the local Universe to $2.32^{+0.54}_{-0.47}$ at $z\approx1$. Interestingly, however, we find that the ratio shows evidence for an increase at higher redshifts, $z > 1$, with  $\langle\rm{M_{Atom}}\rangle/\langle\rm{M_{Mol}}\rangle=5.0^{+1.2}_{-1.0}$  for galaxies with $\langle\textrm{M}_*\rangle\approx10^{10} \ \textrm{M}_\odot$ at $z\approx1.3$. Atomic gas thus clearly dominates the cold-gas content of star-forming galaxies at $z\approx1.3$.

A possible source of error in our $\langle \rm{M_{Mol}} \rangle$ estimates for the CAT$z$1 galaxies lies in the extrapolation of Equation~\ref{eqn:tacconi20} to galaxies with stellar masses $\approx 10^9 \ \textrm{M}_\odot$ at $z \gtrsim 0.7$, a regime that is not tightly constrained by current data \citep{Tacconi20}.
However, {the average $\langle \rm{M_{Mol}} \rangle$ value is dominated by galaxies with $\textrm{M}_*>10^{10}~\textrm{M}_\odot$}. Thus, even if we assume that the molecular gas masses of all galaxies with $\textrm{M}_* < 10^{10}~\textrm{M}_\odot$ are systematically higher by a factor of $\approx 5$ than the values obtained from Equation~\ref{eqn:tacconi20}, this would only increase $\langle \rm{M_{Mol}} \rangle$ at $z \approx 1.3$ by a factor of $\approx 2$, yielding $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Mol}} \rangle \approx 2.5$  and $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Baryon}} \rangle \approx 61\% $. Another possible source of error in the $\langle \rm{M_{Mol}}\rangle$ estimates stems from the uncertainties in the assumptions (e.g. the value of $\alpha_\textrm{CO}$, the dust-to-gas ratio, etc) made when originally determining the molecular gas masses that were used to obtain  Equation~\ref{eqn:tacconi20}; such uncertainties are expected to be $\approx \pm0.25$~dex \citep{Tacconi20}. However, even assuming that the ``true'' molecular gas masses are all 0.25~dex higher than those inferred from Equation~\ref{eqn:tacconi20}, we find that our estimate of $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Mol}} \rangle$ at $z \approx 1.3$ would decrease to $2.8$, and of $\langle \rm{M_{Atom}} \rangle/\langle \rm{M_{Mol}} \rangle$ to $\approx 63\%$. Thus, our conclusion that atomic gas dominates the cold-gas content of star-forming galaxies at $z \approx 1.3$ appears to be robust against even relatively large uncertainties in the average molecular gas mass of high-$z$ galaxies.

Figure~\ref{fig:HIH2} shows that atomic gas is the dominant component of the cold ISM of galaxies at both $z\approx0$ and $z\gtrsim1$. Spatially-resolved H{\sc i} 21\,cm\ and CO studies in nearby galaxies find that the ${\rm H_2}$\ arises in the inner, star-forming, regions of galaxies, while the H{\sc i}\ is much more extended, extending to radii of tens of kpc \citep[e.g.][]{Leroy08}. Indeed, the molecular gas mass dominates the ISM in the central regions of spiral galaxies at $z\approx0$, with the transition from an H{\sc i}-dominated ISM to an ${\rm H_2}$-dominated ISM occurring at approximately half the optical radius, at a characteristic gas surface density of $\approx 14~\textrm{M}_\odot \textrm{pc}^{-2}$ \citep{Leroy08}. For high-$z$ galaxies, CO emission in star-forming galaxies has been found to have a half-light radius of $\lesssim 10$~kpc, similar to the size of the star-forming regions \citep[e.g.][]{Tacconi13,Bolatto15}. Conversely, we find that the average H{\sc i} 21\,cm\ emission from star-forming galaxies at $z\approx1$ is resolved for spatial resolutions  $< 90$~kpc \citepalias{Chowdhury22b}. {It thus appears that the ${\rm H_2}$\ in high-$z$ star-forming galaxies is also restricted to the central high-density regions while the H{\sc i}\ extends out to tens of kpc in a significant fraction of such galaxies.}

In this \emph{Letter}, we have shown that the average atomic gas mass of star-forming galaxies with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$ is comparable to the average stellar mass at $z \approx 1$, and is significantly larger than both the average stellar mass and the average molecular gas mass at $z \approx 1.3$. We find that $\approx70\%$ of the baryonic mass of star-forming galaxies  with $\langle\textrm{M}_*\rangle\approx10^{10}~\textrm{M}_\odot$  at $z\approx1.3$ is in atomic gas. Our results thus demonstrate that atomic gas dominates the baryonic content of star-forming galaxies at $z \approx 1.3$, during the epoch of peak star-formation activity in the universe.

	\begin{acknowledgments}
	We thank the staff of the GMRT who have made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We thank an anonymous referee for a very constructive report that helped increase the clarity of the paper. NK acknowledges support from the Department of Science and Technology via a Swarnajayanti Fellowship (DST/SJF/PSA-01/2012-13). AC, NK, $\&$ JNC also acknowledge the Department of Atomic Energy for funding support, under project 12-R\&D-TFR-5.02-0700.
	\end{acknowledgments}
    \software{ numpy \citep{harris2020array};    matplotlib \citep{Hunter:2007}}

redpajama_set_name: RedPajamaArXiv


On the morning of August 8, 1969, a policeman held traffic outside the recording studio at 3 Abbey Road, in London, so photographer Iain Macmillan could get the iconic shot of the 11th Beatles album, the last they recorded together even though Let It Be was the final album of the band — it had been mostly recorded prior to Abbey Road. He climbed a ladder to take the photographs, and the whole thing only took around 10 minutes. Macmillan credited McCartney in coming up with the idea as he had drawn it out a few days before. He took only six pictures and picked the one where the men's legs were in unison walking across the road.
Because of the quick nature of the shoot and the simplicity of the cover, fans were able to see exactly what was going on that day. Paul McCartney wasn't wearing anything on his feet, opting to take off the sandals he was wearing after the first two shots. There was a group of people in white standing farther up the street, and the license plate number of a Volkswagen Beetle that read "LMW 281 F" was parked on the curb. While it was ironic there was a Beetle on the Beatles album cover, another figure caught in the photograph standing on the sidewalk at the right watching the group had a story all his own.
The man was an American tourist named Paul Cole. He wasn't there because he wanted to get a glimpse of the Beatles. He actually didn't want to follow his wife on their next tourist stop, opting to spend his time outside. He struck up a conversation with the police officer holding up traffic for the photo shoot and saw the four men walking across the street. Cole had no idea who the men were or what they were doing, only thinking that they looked like "a bunch of kooks". Months passed until Cole's wife, who was a church organist, had gotten a copy of the album to play at a wedding. It was then when Cole discovered he was on one of the most famous album covers of all time.
Other rather strange things also spawned from the Abbey Road album. The white Volkswagen Beetle in the picture was stolen multiple times since it was owned by a person that lived in the flats across from the recording studio. It eventually sold at an auction in 1986 for £2,530 and was put on display in a German museum in 2001.
Da Dioniso Punk: dietro le quinte.