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Earn & Learn Students Given the Opportunity to Learn First-Hand About Careers in the Medical Field
Compiled By Milwaukee Courier Staff
Picture provided by Employ Milwaukee Workforce Development
For the second year in a row, Employ Milwaukee has partnered with the Clinical & Translational Science Institute of Southeast Wisconsin (CTSI) at the Medical College of Wisconsin (MCW) to give young people who participate in Mayor Barrett's Earn & Learn Summer Youth Employment Program an opportunity to gain first-hand knowledge of careers in the medical field at one of the most prestigious medical research institutions in the country.
On Friday, August 3, 2018, President and CEO of Employ Milwaukee Willie Wade was the keynote speaker at the CTSI 500 Stars Program closing ceremony at the Medical College, where he congratulated the young people. In his remarks, Wade discussed the importance of innovative partnerships to prepare our future workforce and emphasized the extraordinary opportunity these young people are being given to be able to do a summer internship at MCW/CTSI, and get an early introduction to careers in the medical field. He also thanked the MCW for the great partnership with the Mayor's Earn & Learn Program and Employ Milwaukee.
"I'm excited about our new and growing partnership with the Medical College of Wisconsin. This partnership allows young people who apply to Mayor Barrett's Earn & Learn Summer Youth Employment Program, with an interest in the medical field, to get an up-close look at numerous careers," said Willie Wade, President and CEO, Employ Milwaukee. "We are preparing the workforce of tomorrow by providing one-of-a-kind opportunities to obtain real life work experience. By supporting our young people, we are ensuring a successful future for our community."
MCW is the lead member of the CTSI, a consortium of eight Wisconsin institutions committed to translating biomedical research discoveries into practical patient care and increasing diversity within the clinical and translational science workforce. The CTSI 500 Stars Program introduces young people to careers in clinical and translational science settings through internship opportunities.
"Our goal is to enroll a minimum of 50 under-represented minority students in this Program per year…there is a summer component and an academic year component to 500 Stars; each component has a student-centered activity and a family-centered activity. The summer offers internships and externships at our partner organizations. In the academic year, students enroll in SMART (Students Modeling a Research Topic) teams, and the following summer they come back for internships," said Dr. Reza Shaker, Director of the CTSI and Sr. Associate Dean for Clinical and Translational Science at MCW. According to Dr. Shaker, community involvement in the 500 Stars Program is critical and reflects the team science model of the CTSI. Dr. Doriel Ward, Executive Director of CTSI Administration and Director of the 500 Stars Program concurs and adds, "Our aim for the CTSI 500 Stars Initiative is to provide real-life, practical experiences, in translational science settings as a part of our efforts to train and cultivate the translational science workforce, while also engaging patients, families and community members in every phase of the translational process."
Over the past two summers, 47 Earn & Learn students have participated in the CTSI 500 Stars Summer Internship Program, working in various departments at CTSI partner organizations (including MCW), representing research laboratories, clinical and translational research settings, research administration and support settings, and many more. Moreover, some students took part in the MCW's Apprenticeship in Medicine program for high school students from historically underrepresented backgrounds interested in medical careers. All students received hands-on experience in live settings, participated in enrichment and mentoring activities, weekly translational science lecture series and much more.
Students also had the opportunity to visit the Museum of Science and Industry in Chicago, IL. In the two years of the partnership, the number of Earn & Learn young people has nearly doubled from 17 Earn & Learn participants in 2017 to 30 in 2018.
"We are very pleased with our partnership with Employ Milwaukee," said Joseph E. Kerschner, MD, Dean, MCW School of Medicine; Provost and Executive Vice President. "We are eager to help these young prospective scientists cultivate their passions in multiple medical and clinical fields and look forward to working with Employ Milwaukee to develop the talent of our future workforce."
Popular Interests In This Article: Compiled By Courier Staff, CTSI 500 Stars Program, Earn and Learn, Employ Milwaukee, Medical College of Wisconsin, Willie Wade
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redpajama_set_name: RedPajamaCommonCrawl


"U.S. is withholding $255 Million from Pakistan" – Why are they giving terrorist countries millions of dollars in the first place?
If Congress Just So-Called "Essentially Repealed" Obamacare, Why Pass a Bill to Prop It Up?


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David Vernon "D. J." Reader Jr. (geboren am 1. Juli 1994 in Greensboro, North Carolina) ist ein US-amerikanischer American-Football-Spieler auf der Position des Defensive Tackles für die Cincinnati Bengals. Er spielte College Football für die Clemson University und stand von 2016 bis 2019 bei den Houston Texans unter Vertrag.

College
Reader besuchte die Grimsley High School in seiner Heimatstadt Greensboro, North Carolina, wo er Baseball, Basketball und Football spielte. Ab 2012 ging er auf die Clemson University, um College Football und Baseball für die Clemson Tigers zu spielen. In seinem ersten Jahr am College spielte er als Ersatzspieler sowohl Baseball als auch Football, entschloss sich aber dann, seine Baseballkarriere zu beenden und sich auf Football zu konzentrieren. Anschließend spielte er drei Jahre lang Football für die Tigers und erzielte dabei 72 Tackles, davon neun für Raumverlust, und vier Sacks. Nach dem Tod seines Vaters setzte Reader die erste Hälfte der Saison 2015 aus persönlichen Gründen aus.

NFL
Reader wurde im NFL Draft 2016 in der fünften Runde an 166. Stelle von den Houston Texans ausgewählt. Als Rookie kam er in allen 16 Spielen zum Einsatz, davon siebenmal als Starter. Dabei erzielte Reader in der Regular Season 22 Tackles und einen Sack. In seinem zweiten NFL-Jahr wurde er nach dem Karriereende von Vince Wilfork zum Stammspieler auf der Position des Nose Tackles. In den nächsten drei Spielzeiten bestritt Reader 45 Spiele für die Texans. Insgesamt kam er in vier Jahren für Houston auf 173 Tackles, davon 17 für Raumverlust, und 6,5 Sacks.

Im März 2020 unterschrieb Reader einen Vierjahresvertrag im Wert von 53 Millionen US-Dollar bei den Cincinnati Bengals. Am fünften Spieltag der Saison 2020 zog er sich einer Oberschenkelverletzung zu, wegen der er für den Rest der Saison ausfiel. In der Saison 2021 zog Reader mit den Bengals in den Super Bowl LVI ein, den sie mit 20:23 gegen die Los Angeles Rams verloren. In der Spielzeit 2022 verpasste Reader verletzungsbedingt sechs Spiele.

NFL-Statistiken

Einzelnachweise

American-Football-Spieler (Clemson Tigers)
American-Football-Spieler (Houston Texans)
American-Football-Spieler (Cincinnati Bengals)
US-Amerikaner
Geboren 1994
Mann

redpajama_set_name: RedPajamaWikipedia


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Penllyn (cantref)
Penllyn (head of the lake i.e. Bala Lake or Llyn Tegid) was a medieval cantref originally in the Kingdom of Powys but annexed to the Kingdom of Gwynedd. It consisted of the commotes (cymydau) of Edeyrnion, Dinmael, Penllyn is Treweryn and Penllyn uwch Treweryn (is signifying 'below' and uwch 'above' the River Tryweryn).
Medieval commotes of Wales
On the north and west it bordered Gwynedd (the cantrefi of Tegeingl, Rhufoniog, Dunoding and Meirionydd); it bordered the Powys cantrefi of Maelor, Mochnant and Cyfeiliog on the east and south.[1]
After the death of Madog ap Maredudd, the last Prince of the whole of Powys, and his eldest son and heir in 1160, the kingdom was divided between his surviving sons Gruffydd Maelor, Owain Fychan and Owain Brogyntyn, his nephew Owain Cyfeiliog and his half-brother Iorwerth Goch.[2] Penllyn was inherited by Owain Brogyntyn; Edeyrnion had been the home of his mother (who was not married to his father) and he may also have been raised there.
The military skill and strength of Madog had prevented Gwynedd from asserting hegemony over Powys, but following Madog's death, it was able to force Owain Brogyntyn to become a vassal. Penllyn was thus annexed to Gwynedd.
Following the eventual defeat of Gwynedd by English forces, and the consequent Statute of Rhuddlan, it became part of Merionethshire
^ Rees, William (1951). An Historical Atlas of Wales from Early to Modern Times. Faber & Faber.
^ Ashley, Mike (2012). The Mammoth Book of British Kings and Queens. Hachette.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Penllyn_(cantref)&oldid=876383502"


The 1776 Foundation is a non-profit research and education association created to inform and equip the people of Montana to better evaluate policy options that uphold traditional American values, historic civil liberties, the Montana Constitution, and the Constitution of the United States of America.
Every day we strive to help our neighbors in need of assistance with integrity and compassion through our Crisis Fund. By purchasing our plate, you can be assured your donation is making a difference between hope and despair. We support families and individuals with financial assistance when faced with a crisis they never expected. Your generosity will enable us to fulfill our mission one plate at a time, one crisis at a time.
This plate benefits Yellowstone Public Radio. YPR generates funds to help pay for programming which is heard throughout most of the State of Montana.
Our mission is to improve the quality of care and life for children with bleeding disorders, including hemophilia and Von Willebrand disease through education, peer support, resources, research and referral.
This plate benefits survivors of Law Enforcement officers who have died in the line of duty. The funds will be used for support services for family members and affected coworkers.
This plate helps the Montana Contractors' Association Education Foundation provide scholarships to develop a pipeline of committed, quality workers for Montana's construction industry.
The Montana Crime Prevention Association is a professional organization and encompassing community representation at all levels dedicated to providing collaborative partnerships and education that addresses, encourages, and supports crime prevention efforts in Montana. We exist to promote comprehensive awareness about the role that effective crime prevention plays in improving the quality of life for all.
Please contact the sponsor for information about the organization and how it uses donations from plate sales.
This plate supports the community foundation and its effort to support local projects and non-profit work in Sweet Grass County.
This plate helps Montana families flourish by providing exciting, educational activities through museums and other similar projects. These facilities provide a platform for discussion, interaction and education where individuals can connect and learn.
Compassion Montana exists to bridge the gap between the aid worker and the work field. We are a local nonprofit providing assistance needed to make volunteering possible for people who are willing to give their time and use their talents to help where they are needed most.
The funds from this plate help us accomplish our humanitarian mission of bringing hope to the hopeless and stability to the unstable while teaching morality and work ethic along the way. We connect directly with people in distressed areas to solve real problems as quickly, inexpensively and intelligently as possible. Visit our website for more information.
This plate benefits local CASA programs that train volunteers to advocate for children in the abuse and neglect system. The CASA program provides awareness and education on the child abuse issue in Montana.
This plate benefits the Montana Food Bank Network and will help their mission to end hunger in Montana through food acquisition/distribution, education and advocacy. They partner with over 280 network partners that are food banks, food pantries, shelters, senior centers and schools to improve food access and share information to address hunger and its root causes.
This plate will generate funds for the upkeep and maintenance of the Veteran's Monument in Hamilton, MT., which honors those who have served in the armed forces. (veteransmonument.org) The plate will also generate funds for helping Veterans in need.
Everyone is eligible to purchase this plate. This plate benefits Rural Fire Districts and Fire Service Areas throughout Montana by providing information and assisting communications between Rural Fire Trustees, Volunteer Firefighters, and the communities they serve.
This plate benefits the Montana Pilots Association's efforts to promote general aviation within the State of Montana. This plate generates funds to provide aviation scholarships as well as preserve and maintain Montana airstrips.
This plate benefits police officers and their families that have been injured or killed in the line of duty, scholarships for children of police officers, law enforcement Torch Run for Special Olympics, and Montana Operation Life Saver.
This plate funds our programs to provide hope through humanitarian aid. Our work strengthens struggling families, protects disadvantaged children, demonstrates American generosity, and promotes a path to self-reliance and resilience.
Funds generated from plate sales go to care, support, research, awareness and advocacy activities.
Show your support with Montana's Stop Diabetes license plate! Your purchase of this plate includes a $30.00 tax-deductible donation to support the American Diabetes Association's research, education, and advocacy. Work in Montana for children and adults with diabetes. Funds will also provide scholarships for Camp Montana, a camp dedicated to children and teens with Type 1 Diabetes.
This plate benefits Ecology Project International, a non-profit organization that operates science education programs for middle and high school youth in Montana. This plate generates funds for student participate in field ecology, wildlife research, and conservation education programs.
Funds collected from this program will be used to provide facilities and programs for the development of quality, affordable and disciplined competitive and recreational skating opportunities. Proceeds will help expand centrally located programming and facilities operated by Bozeman Amateur Hockey Association with benefits skaters throughout the state and region.
This plate generates funds for promotion, education and training that enhance the safety and welfare of workers throughout Montana.
This plate helps to pay for infant funerals in the state of Montana.
This plate supports volunteer firefighters in Montana. Funds will be used to purchase equipment, provide training, education and support firefighting activities.
Money from every license plate purchased goes to the Benefis Healthcare Foundation for the Mercy Flight Fund.
This plate benefits people who bicycle or walk in Montana. The plate generates funds for public awareness and education programs to increase safety and encourage people to bicycle and walk.
This plate funds our efforts to work hand in hand with those who are bringing humanitarian aid and hope to people in need around the world. Our goal is to help families grow up healthy and happy, and to help create strong communities and partners to ensure this can happen.
All proceeds benefit Montana families affected by cancer.
Chicks n Chaps is dedicated to providing funding for the direct benefit of individuals fighting breast cancer in our local Montana communities while promoting breast cancer awareness through the western lifestyle. Money raised in Montana stays in Montana.
Child Bridge Montana is a faith-based nonprofit that works with churches, the community, and government to create awareness of the need for families to foster and adopt children from the Montana foster care system.
(A motorcycle license plate.) Donations are for the Department of Justice Chrome for Kids Wish Fund grants that fund efforts by Montana-based nonprofit corporations to grant wishes to chronically or seriously ill Montana children. 2017 recipients are: Montana Hope Project; Make-A-Wish® Montana; Cancer Support Community Montana.
This plate supports the health, wellness and safety of children and families in Western Montana through the initiatives of Foundation for Community Health, successor organization of Community Medical Center Foundation. The Foundation provides philanthropic support of the advancement of healthy lives in Western Montana.
NOTE: This plate is available to the general population regardless of military status. Please be advised that because this is a specialty plate and not a military plate, emblems such as "Disabled Veteran" cannot be added and veteran exemptions do not apply. See MCA 61-3-458 through -460 for additional information on veteran plate types and exemptions.
Funds support the Department of Montana VFW Service Office, which assists veterans and their dependents in applying for and receiving federal, state, and local benefits including medical care, compensation, pensions, burials, education, vocational rehabilitation, and employment services; and, advocates for them before Veterans Affairs and the Board of Veterans Appeals.
This plate benefits DEAP a not for profit organization providing services individuals with autism and their caregivers including public awareness and education, evaluation and diagnosis and applied behavioral intervention.
Disability Rights Montana protects and advocates for the human, legal, and civil right of Montanans with disabilities. All funds generated from the plates will support training and advocacy to people with disabilities. Everyone is eligible to purchase this plate.
This plate benefits organizations throughout the state that serve people with disabilities and children with cancer.
Funds generated provide support to Montana firefighters, enabling them to participate in education programs, training, scholarships, and Montana Mutual Aid. Everyone is eligible to purchase this plate.
Habitat for Humanity of Gallatin Valley, Inc.
This plate benefits Habitat for Humanity organizations throughout Montana to help qualified families obtain and remain in decent, affordable housing in our communities.
IC3 MT supports the development of youth cycling access all ability levels through the disciplines of road, mountain and cross riding, training and racing. Additionally IC3 MT supports other charitable organizations and events statewide.
The Jeannette Rankin Peace Center exists to connect and empower people to build a socially just, nonviolent, and sustainable community and world.
Proceeds from the sale of this plate will be used exclusively to fund the Montana NICU Family Support Program. This program provides education and support to parents of sick and premature babies and the staff that care for them in the neonatal intensive care unit.
Money earned from plate sales goes to scholarships.
Funds from the specialty plates are placed in our organization's endowment fund to be used for education and public awareness of the wide range of services we provide to senior citizens to help them live as independently as possible for as long as possible.
The goal of the Hope Project is to make dreams come true for critically ill children in Montana. It raises money through fundraisers, corporate donors, donations and memorials, and ninety percent of all proceeds raised go directly to Montana children. The most requested wish is a trip to Walt Disney World.
All proceeds from the sale of these plates will support MLA and its projects highlighting Montana libraries.
The Montana Lions Sight & Hearing Foundation serves all Lions Clubs and citizens of the State of Montana. The Foundation uses the specialty license plate funds to provide assistance to citizens of Montana with a financial need and a documented medical need associated with sight, hearing and/or speech impairments.
Funds collected from the sale of our license plates are used within the mission of our Foundation: to dispense charity, both public and private, and encourage and promote free public education and schools through endowments, grants, scholarships and fellowships, and to support charitable, scientific, literary or educational purposes.
This plate benefits the Montana State Alliance of YMCAs and our mission to put Christian principles into practice through programs that build a healthy spirit, mind, and body for all. Includes YMCAs in Billings, Bozeman, Butte, Dillon, Helena, and Missoula.
Authorization from organization required for purchase. Contact sponsor for requirements/required documents.
Support our Troops® is a nonpartisan, nonpolitical organization founded to help citizens and community-minded businesses find constructive ways to show their patriotism and appreciation for those that sacrifice so much. All donations are used to bring aid and comfort to our troops in the field and their families at home.
The Montana Utility Coordinating Council promotes safe digging through the Montana811 Call Before You Dig system. The funds obtained through the plates are used for promotional materials, advertising, education, and presentations to promote safe digging to excavators throughout Montana to protect Montanans from accidental damage to an underground utility.
Neighbor to Neighbor is a northwest Montana 501(c)(3) advocacy group promoting S.A.F.E. in our neighborhoods. Safety, Assistance, Friendship & Endowments. We take great pride in our community and look forward to creating secure and crime-free neighborhoods.
Purchasing this plate ensures that Planned Parenthood of Montana continues to provide the highest quality health care services, education, and advocacy so that all people have the freedom to manage their own sexual and reproductive health.
Contact sponsor for required application. Annual recertification also required.
This plate is a way for Montana EMS personnel to proudly display their role in emergency medicine. It was designed for recruitment, retention, statewide morale and identification on scene. Funds generated are given as grants to assist with keeping Montana EMS current with training, equipment and other necessary education.
Tough Enough to Wear Pink (TETWP) of Montana is dedicated to providing funding for breast cancer awareness, education, screening, support and further diagnosis for Montana women and men.
This plate will benefit the United Property Owners of Montana (UPOM) and their efforts to educate the public about the importance of private property rights and will generate funds to be used for the purpose of uniting property owners across Montana to protect and preserve private property rights.
This plate benefits the Violence Free Crisis Line, which works to end domestic violence and sexual assault by empowering individuals and families who have experienced physical, emotional, or sexual abuse. We also work to cultivate communities free from violence through education and community outreach.


At Lombana Hoelle Trial Law, we are passionate about the practice of law. We are dedicated to protecting our clients' rights and achieving successful results. Our legal team provides experience and professionalism across numerous legal disciplines combined with a focus on the unique individual, business and personal requirements of our clients. We offer you effective legal counsel, timely response and an optimal level of professional dedication and integrity.
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Our attorneys possess the necessary talent and experience to navigate a diverse legal landscape. This approach leads to effective and efficient legal representation and, therefore, positive outcomes regardless of whether in the courtroom or at the negotiating table.
We are advocates for individuals who face catastrophic personal injury or medical malpractice. Lombana Hoelle Trial Law represents individuals and corporations in both state and federal courts in high-stakes complex commercial disputes.
Lombana Hoelle Trial Law will never compromise what is right and just for our clients.


The end of an era is approaching. With six NFL quarterbacks projected to be starters this year, we could see a lot of players retire after this upcoming season. So many stars from the past are possibly heading into their final year of the NFL, while some others at an old age will likely continue to play. And a big part of why these players may retire, is due to the young talent that is up and coming.
When there's young talent coming up, it forces teams to start over and prepare for the next 10-15 years. You can develop a team around the veteran players for so long, until you realize you need to move forward without them. A large portion of the league has very young quarterbacks starting, or getting prepared to start for 2019. It's the way the league is.
Some teams like the Dallas Cowboys and Philadelphia Eagles have adapted by going younger. And usually when you go younger, you can acquire more players because the contracts are cheaper. But when you have to pay a player over 30 at least $10 million a year, it may not be worth it. So, the question is, what NFL players are going to leave the game behind in 2018, and who will stay?
It's a good thing to thing about because we could be watching the final season for many stars. Nobody would have even thought that the 2017 season would be the last ever season Jason Witten suits up in a Cowboys jersey. Surprises happen, and many of them may happen after this season.
The most likely player to retire, is Jay Cutler. Cutler originally retired before the 2017 season, but decided to come back when the Dolphins offered him a starting job. While he's heading to television, he may wait until the end of the 2018 season after he realizes no team wants to sign him.
With it being preseason, there's still plenty of time for a quarterback to get hurt, which could give him another opportunity to play again.
It may be an opportunity for him to come back and shine one last time. If not, he will move on.
Another player in limbo right now, is Alfred Morris. It's shocking that Morris is a free agent, considering how well he played with the Dallas Cowboys. A big reason why many believe the Cowboys didn't re-sign him, was because of how expensive he may be. But for some reason, there hasn't been much interest in him.
As the preseason begins, Morris will find interest. He likely won't find any better than a one-year deal, which may be the last of his career. After seeing Darren McFadden retire last season, Morris may follow McFadden's footsteps after the 2018 season comes to an end.
Kickers tend to be the oldest players in the NFL, since they don't have to deal with any contact. Matt Bryant is 43 years old, still kicking for the Atlanta Falcons. Bryant is a lot older than most NFL players, so many would expect him to retire at such an old age in football terms. But after Bryant signed a three-year deal this offseason with the Falcons, he still has some time left in the league. Bryant may aim to be the oldest player in the NFL by the time his contract comes to an end. Lucky for the Falcons, he's been accurate throughout his career.
The oldest player in the NFL currently is Adam Vinatieri, who seems like he will be in the last season of his NFL career. Vinatieri signed a one-year this offseason with the Colts, which should be the last contract of his career.
Heading into his 23rd season in the NFL, Vinateri has had a remarkable career with countless game winning field goals.
Chances are, Vinatieri came back for one more season in hopes that Andrew Luck could come back to take the Colts to the playoffs. Who doesn't want to win on a high note? And if it doesn't happen, he moves on with his life.
Ray Lewis decided to wait until the Ravens won another Super Bowl to retire, so what will it take for another great Ravens linebacker, Terrell Suggs, to retire? The Ravens may not win another Super Bowl anytime soon, but it's unlikely that he will retire on a losing team.
After drafting Lamar Jackson, there is hope that this team can be successful again. Jackson won't get any playing time at quarterback this season, but Suggs will at least stay around for one season while Jackson is the starter, to see if he can turn this organization around. Give it until at least 2020 before Suggs decides to retire.
Even at 34 years old, Brent Grimes has been an aggressive cornerback. Since 2013, Grimes has had at least four interceptions each season. But going into his 12th season at 35-years old, there's a time to move on. Grimes signed a one-year deal with the Buccaneers, and has debated retirement in the past. The Buccaneers likely won't be successful this season with the weak secondary and suspension of Jameis Winston. And no one is going to want to sign an aging cornerback. Look for Grimes to give it his all in final season with the Buccaneers.
Although Adrian Peterson probably should've retired a couple of years ago, he's still seeing interest from teams this summer.
The New Orleans Saints have mentioned that they would be interested in bringing back Peterson, especially after Mark Ingram got suspended for the first four games of the season.
And honestly, Peterson had a couple of games last season where he looked like himself. Before Alfred Morris gets signed, Peterson has to, for one last season. He's going to look for a team that he can possibly win a Super Bowl with for his final season, before he decides to retire in 2019.
Sometimes, players choose to come back for another season because the previous season wasn't worth going out on. Brandon Marshall missed most of the 2017 season due to an injury he suffered with the New York Giants. Now signing a one-year deal with the Seahawks, it gives him a great chance to be a big part of this offense, going out strong.
Marshall has opportunities to work on television, so he can retire and be guaranteed a job after retirement. Marshall will give it all he has for a team that he can be a starter with, and whatever happens from there, happens.
Unless the New Orleans Saints win the Super Bowl this season, Drew Brees will be back in 2019. Brees signed a two-year deal with the Saints this offseason worth $50 million. So Brees is definitely in it for another two seasons. It seems obvious, but many fans still may believe that he will call it quits after this season. At some point, players want to move on. But, Brees arguably has the best team he's had throughout his career.
He has a defense that is improving, and it's the best run game the Saints have had in his career. For once, Brees does not need to carry the team on his own.
Antonio Gates' 2018 season is still up in the air, considering he's still a free agent. But with the success he's had throughout his career, he shouldn't have any issues signing at least a one-year deal.
The Los Angeles Chargers seem to be interested considering Hunter Henry will miss the 2018 season due to a torn ACL.
Other teams that could be interested include the Dallas Cowboys and Miami Dolphins. The point is, he should play in 2018, and he wants to. But it would be his last season. One more chance to possibly win a championship, something he was never able to do with the Chargers.
Josh McCown has the best contract of his career, as he signed a one-year deal worth $10 million to re-sign with the Jets. Coming off of the best season of his career, it makes sense for McCown to come back one more time and cash out. But with Sam Darnold breathing down his neck, this will for sure be his last season.
After suffering a broken hand in 2017, he's a tough hit away from ending his career. It's not easy to be a 39-year-old quarterback and take all these hits, unless you're Tom Brady. McCown won't go out under the spotlight, but he will go out playing the best football of his career.
Retirement plans were put on hold for Julius Peppers, as he decided to come back for one final season with the Carolina Panthers. Hearing the talks of it, it almost seems certain that Peppers will not be back in 2019. 38-years old is difficult for a defensive end, especially with all the young offensive tackles in the league.
The Panthers are extremely inconsistent, and have struggled every other year. This year would be a struggle, and Peppers is going to get fed up. This season, Peppers will realize how tough it is at his age to keep playing, and choose to step away from the game in 2019.
No matter how bad an offensive line is, Frank Gore manages to play well each season. New teams haven't been a problem for him, as he continues to play well. Gore is fifth on the all-time rushing list with 14,026 yards, and should easily pass Curtis Martin, as he only needs another 75 yards.
Gore will play at least two more years to make his way up in the history books, but to also possibly win a championship.
Gore played in one Super Bowl, but may choose to see how free agency goes in 2019, where he may have a better chance of signing with a better team who can give him the success he wants.
The oldest active defensive player, may be no more. Terence Newman signed a one-year deal with the Vikings, to probably finish off his career in Minnesota. Newman will turn 40 years old before the 2018 season starts, which is pretty impressive as a cornerback.
Newman's playing time is going down as he gets older and his effectiveness decreases. A big reason why he probably wanted to come back was seeing how close the Vikings are to winning a championship. Regardless of how this season goes, it makes sense why Newman wouldn't want to end his career by getting blown out in the NFC Championship Game.
Although Beast Mode really ended in 2014, Marshawn Lynch is playing his final career in Oakland this season. Lynch may try to come back in 2019, playing the final season the Raiders play in Oakland, but with the new direction the team is going, it is highly unlikely Jon Gruden will want to bring him back.
Lynch and Doug Martin will share carries in 2018, but the team will probably look for a future running back as time goes on. Lynch already retired once, so it's a matter of time before he hangs the cleats up once again. He only came back to the NFL to play for his hometown Raiders, and with the Raiders' impending move to Las Vegas, Lynch's career is in its twilight.
On the field, Rob Gronkowski is the best tight end in the game right now. Actually, he also may be one of the best pass catchers in the game. But, being that big of a target comes taking a lot of tough hits, that have clearly affected Gronkowski.
The injuries Gronkowski has suffered have made him debate retirement for some time, but 2018 will be the year.
There have been so many speculations on when the end of Gronkowski will come, but this may be the end of the Patriots era. There is no way Gronkowski will want to play another season risking injuries in 2019.
Retiring after this season would make no sense for Larry Fitzgerald. If he retired after the 2017 season, it would have made sense because Carson Palmer did so, as did coach Bruce Arians. But this is really a transition season with signing Sam Bradford, while also drafting Josh Rosen. There's no way the Cardinals draft Rosen and Fitzgerald decides to retire before he becomes the starter.
Fitzgerald will be turning 35 years old before the season starts, so retirement will be coming soon. But he could shock everyone and play another 2-3 seasons, in hopes of winning a championship. It all comes down to how good Josh Rosen will actually be.
Tony Romo won't be the only future Hall of Famer who retires without a Super Bowl ring. Philip Rivers has been one of the best quarterbacks in the NFL throughout his career, but may have to retire without a ring. And right now, he's the odd man out. The Chargers are building a young team around him, and he's the old man.
Obviously, Rivers isn't holding the Chargers back from winning, but they still have a few more years before they can legitimately compete. Unfortunately, Rivers has been stuck in a conference with so many great quarterbacks that have the help they need in order to be successful.
That's right, Ben Roethlisberger will retire after this upcoming season. As great as he's been, this team could possibly lose their franchise running back after this season. Le'Veon Bell has had difficulties landing the long-term deal he's been looking for. And quite frankly, he may not sign it.
Roethlisberger has also shown signs of wanting to retire, and he will finally make the move.
The frustration will hit him when the Steelers are unable to make it to the Super Bowl, with the Patriots blocking their way.
Roethlisberger will have had enough, and move on with his life. The best Steelers offense in it history may not have what it takes to win a championship.
The end of an era. Tom Brady will retire after the 2018 season. Talks of Brady retiring have been circulating for a while, but it seems like Brady can only go for so long until there's no point in playing. Many teams are extremely talented, but you can never count the Patriots out when it comes to the Super Bowl. However, NFL QBs declining usually happens quickly. Just look at how quickly Peyton Manning or Brett Favre declined once they turned 40. We also can't count out the lingering tension in New England between Brady and Bill Belichick, who reportedly wanted to move on to Jimmy Garoppolo this season, had he not been forced to trade him.


On the other side of the issue, Planned Parenthood Federation of America is continuing to lobby the Senate against including the Stupak language. On Wednesday, leaders from 11 pro-choice groups lobbied on the Hill.
Two senators who have voted against abortion rights — Sen. Bob Casey (D-Pa.) and Sen. Kent Conrad (D-N.D.) — did not raise any detailed objections to the abortion language, but both said they were still reviewing it.
Most senators said they had yet to read through the entire bill — or the summaries that their staff members were preparing. Reid's plan would expand coverage to 94 percent of Americans through a government-run health insurance option — allowing states to opt out — and other features, all while reducing future federal deficits by $130 billion during the next 10 years, according to a Congressional Budget Office report.
"I just like the numbers," said Sen. Claire McCaskill (D-Mo.), who pledged to read "every word." "I love the deficit reduction.
"This is a lousy bill that is going to cost American taxpayers like mad for the rest of their lives, if they happen to pass it. I hope the American people rebel," Hatch said Thursday morning on Fox News Channel. Landrieu said she was still studying the bill Thursday, and she would not decide on her vote until Friday at the earliest.
She said she was still concerned about making insurance affordable for lower-income people and was disappointed the new insurance exchanges wouldn't start until 2014.
Nelson continued to draw a distinction between the vote on the motion to proceed and the vote to end debate after the amendment process — an argument that has given Democrats hope that they will get 60 votes Saturday.
Reid said he maintains a dialogue with Maine Republican Sens. Olympia Snowe and Susan Collins, hoping to secure some hint of bipartisanship in the future.


text:
\section{Introduction}
\emph{Gaia}{} \citep{gaiacollaborationGaiaMission2016}, especially data release 2 (DR2; \citealp{gaiacollaborationGaiaDataRelease2018a}), which included radial velocities, has revealed the Galactic disk to be dynamically complex \citep{gaiacollaborationGaiaDataRelease2018b, antojaDynamicallyYoungPerturbed2018}.
Many perturbers are at play, and the specific influence of each is not yet clear.
The Galaxy's bar (e.g. \citealp{huntOuterLindbladResonance2018a, fragkoudiChemodynamicsBarredGalaxies2019}), spiral structure \citep{quillenSpiralArmCrossings2018, kawataRadialDistributionStellar2018,huntTransientSpiralStructure2018, antojaDynamicallyYoungPerturbed2018,sellwoodDiscriminatingTheoriesSpiral2019, khannaGALAHSurveyGaia2019, khoperskovHicSuntDracones2020}, and satellite galaxies \citep{laporteFootprintsSagittariusDwarf2019, khannaGALAHSurveyGaia2019} all affect disk kinematics.
Furthermore, \citet{huntSignaturesResonancePhase2019} showed that the signatures of each are difficult to disentangle and that many interpretations of the data are possible. \citet{hilmiFluctuationsGalacticBar2020} showed that perturbers can interact significantly, further complicating matters.

In this work, we focus on the chemical signatures of the bar in action space, and demonstrate that chemical abundances can aide the identification of bar resonances in the disk and constrain the bar pattern speed, $\Omega_\text{p}$.
Because most abundances do not change over a star's lifetime, they trace its birth location, providing a non-dynamical ``memory'', that can help distinguish the effects of disk perturbations.
Past work on chemistry and dynamics has examined the distribution of metallicities and ages near the Sun or throughout the disk to constrain radial migration (e.g. \citealt{schonrichChemicalEvolutionRadial2009, haydenCHEMICALCARTOGRAPHYAPOGEE2015, martinez-medinaRevealingSpiralArms2016, khoperskovEscapeesBarResonances2019, frankelKeepingItCool2020}).
Recently, \citet{chibaTreeringStructureGalactic2021} examined the chemical signature of a decelerating bar.
We emphasize the importance of the spatial selection function and the limited azimuthal coverage of current datasets.

The existence of the Milky Way's bar was first inferred from gas velocities \citep[e.g.][]{devaucouleursInterpretationVelocityDistribution1964, cohenObservationsOHGalactic1976, lisztGasDistributionCentral1980}, then with photometry \citep{blitzDirectEvidenceBar1991, weilandCOBEDiffuseInfrared1994} and star counts \citep[e.g.][]{nakadaBulgeOurGalaxy1991, whitelockShapeBulgeIRAS1992, weinbergDetectionLargescaleStellar1992}.
Over time, its pitch angle has been constrained, with the modern consensus being that the bar is ahead of the Sun by roughly $27^\circ$ \citep{dwekMorphologyNearinfraredLuminosity1995, binneyPhotometricStructureInner1997, stanekModelingGalacticBar1997, lopez-corredoiraBoxyBulgeMilky2005,  rattenburyProperMotionDispersions2007, caoNewPhotometricModel2013, weggMappingThreedimensionalDensity2013}.
The bar's pattern speed, however, is still disputed.
Identifying the Hercules moving group, a feature of the local velocity distribution, with the Outer Linblad Resonance yields a pattern speed of roughly $55~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$ (\citealp{dehnenPatternSpeedGalactic1999, dehnenEffectOuterLindblad2000}, later \citealp{chakrabartyPhaseSpaceStructure2007, minchevNewConstraintsGalactic2007, minchevLowvelocityStreamsSolar2010, antojaConstraintsGalacticBar2014, fragkoudiRidgesUndulationsStreams2019a}).
On the other hand, studies of the inner Galaxy suggest that the bar is slower, with a pattern speed of 30--40 $\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$ \citep{weinerPropertiesGalacticBar1999, rodriguez-fernandezGasFlowModels2008, longMadetomeasureGalaxyModels2013, weggStructureMilkyWay2015, sormaniGasFlowBarred2015}, and that Hercules could be due to the CR resonance \citep{perez-villegasRevisitingTaleHercules2017, monariTracingHerculesGalactic2019, monariSignaturesResonancesLarge2019, binneyTrappedOrbitsSolarneighbourhood2020}.
Recent studies suggest a figure around the upper end of this range \citep{portailDynamicalModellingGalactic2017, clarkeMilkyWayBar2019, sandersPatternSpeedMilky2019, monariSignaturesResonancesLarge2019, bovyLifeFastLane2019}.

\subsection{Dynamical background: axisymmetric actions and resonances} \label{sec:background}

The primary way the bar impacts the disk is through resonant trapping, which affects stellar orbits with frequencies commensurate with the bar, i.e. for which
\begin{equation} \label{eq:res}
    m(\ensuremath{\Omega_\text{p}} - \Omega_\phi) \approx l \Omega_R \quad ,
\end{equation}
where $m$ and $l$ are small integers with $m > 0$, and $\Omega_\phi$ and $\Omega_R$ are the frequencies of azimuthal and radial oscillation, respectively.
These orbits librate around their parent orbits, which are closed in the frame that rotates with the bar \citep{contopoulosOrbitsBarredGalaxies1989, athanassoulaMorphologyBarOrbits1992}.

Stars trapped at corotation (CR; $l=0$) exhibit oscillations around a constant azimuth with respect to the bar.
Typical galaxy bars have a dominant Fourier $m=2$ mode \citep{butaFourierDissectionEarlyType2006}, which means that $m=2$ resonances, especially the Outer and Inner Lindblad Resonances (OLR and IRL), with $l=\pm1$ and $m=2$, affect the disk strongly.
Those with $l = \pm 1$, $m = 1$ and $l = \pm 1$, $m = 4$ (referred to as 1:1 and 1:4, respectively) are generally present, but much less dominant, unless the Fourier $m=4$ mode of the bar is strong \citep{huntOuterLindbladResonance2018a}.

While the true potential of the Milky Way is complex, asymmetric, and time-dependent, we can use an axisymmetric approximate potential model to calculate ``axisymmetric actions extimates'', $J_\phi, J_R, J_z$, for each star, associated with azimuthal, radial, and vertical motion, respectively \citep[e.g.][chapter 3]{binneyGalacticDynamicsSecond2008}.
The frequencies of these oscillations follow from the Hamiltonian $H_\text{axi}$ as
\begin{equation}
    \Omega_{\text{axi},i} = \frac{\partial H_\text{axi}}{\partial J_i} ; \quad i \in \{\phi, R, z\} \quad ,
\end{equation}
which are the same as those in Equation \ref{eq:res} only when the true potential is exactly axisymmetric.
From here on, we refer to axisymmetric action estimates simply as \emph{actions}.
Unlike true actions, which are conserved but not generally known, these change as the star orbits in a non-axisymmetric potential \citep[e.g.][]{lynden-bellGeneratingMechanismSpiral1972, sellwoodRadialMixingGalactic2002, binneyOrbitalToriNonaxisymmetric2018, trickIdentifyingResonancesGalactic2021}.
Stars on orbits resonant with the bar and with small $J_z$ oscillate around negatively-sloped lines in the $J_R$--$J_\phi$ plane, with $J_R$ decreasing with increasing $J_\phi$ along them \citep{sellwoodRecentLindbladResonance2010}.
We refer to these as axisymmetric resonance lines (ARLs).

Because of the conservation of the Jacobi integral, changes to the axisymmetric actions of stars obey
\begin{equation}\label{eq:jjlm}
    \Delta J_R = \frac{l}{m} \Delta J_\phi
\end{equation}
to first order \citep{lynden-bellGeneratingMechanismSpiral1972, sellwoodRadialMixingGalactic2002}.
Consequentially, corotating stars can undergo changes to their angular momentum, $J_\phi$, without being radially heated.
Most stars are on near-circular orbits, meaning that scattering at the outer 1:1, 1:4, and 1:2 Linblad resonances preferentially increase eccentricity, $J_R$, inducing a net outward migration and leading to under- and over-densities on either side of the ARL.
See \citet{trickIdentifyingResonancesGalactic2021} for a pedagogical introduction and numerical investigation of these effects.
Evidence of these processes can be seen in velocity- and action-space density.
In this work we investigate the signatures of bar resonances in joint action-metallicity space.
We also show that this depends strongly on the location of observed stars, i.e. the spatial selection function.

In sections \ref{sec:data} and \ref{sec:sims} we describe the observational data and simulations we use, respectively.
In section \ref{sec:results}, we show how bar resonances give rise to distinct chemical signatures and compare them to observations.
In section \ref{sec:discussion}, we discuss the impact of spatial selection functions and consider the capabilities of future surveys.
We conclude in section \ref{sec:conclusions}.

\section{Data}\label{sec:data}
\begin{figure}
    \centering
    \includegraphics{gaia_lamost_footprint.pdf}
    \caption{The radial distribution of LAMOST\ and \emph{Gaia} RV{} stars.  LAMOST\ RVs can fruitfully augment \emph{Gaia}\ in the outer disk.}
    \label{fig:footprints}
\end{figure}

We use astrometry from \emph{Gaia}\ EDR3 \citep{gaiacollaborationGaiaEarlyData2020}, which includes positions, parallaxes, and proper motions for $1.3 \times 10^9$ sources, as well as radial velocities (RVs) for $4 \times 10^6$ stars (hereafter the \emph{Gaia} RV\ sample; these are the same as in DR2).
We also use the LAMOST\ \citep{cuiLargeSkyArea2012, zhaoLAMOSTSpectralSurvey2012, dengLAMOSTExperimentGalactic2012a} DR 5 FGAK sample, which provides RVs and metallicities for $4.2 \times 10^6$ stars from low-resolution ($R \approx 1800$) spectra.

In order to focuss the investigation on near-circular in-plane disk orbits, we used only stars with $J_z < 10~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ and $|z| < 1~\ensuremath{\mathrm{kpc}}$.
This selection is dominated by thin disk, low-alpha sequence stars.
We also removed the $\sim1\%$ of stars with $L_z$ outside $1000 - 3000~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ to facilitate comparison with simulations.
In order to mitigate magnitude-driven selection effects, we use only LAMOST{} giants with $2.2 < \log g < 2.7$ and $4500~\mathrm{K} < T_\mathrm{eff} < 5000~\mathrm{K}$ when dealing with abundances, which often have stellar-parameter-dependent systematics.
These cuts leave roughly 800,000 stars when abundances are not needed, and 95,000 when they are.

Future \emph{Gaia}\ data releases will include more RV measurements, but at present, the \emph{Gaia}\ catalog can be usefully augmented with LAMOST\ RVs, despite the fact that the latter has a larger typical uncertainty ($\sim5~\ensuremath{\mathrm{km~s^{-1}}}$, as opposed to \emph{Gaia}'s $\sim1~\ensuremath{\mathrm{km~s^{-1}}}$).
Figure \ref{fig:footprints} shows the radial distribution of LAMOST\ and \emph{Gaia} RV\ stars.
While there are far more \emph{Gaia} RV\ than LAMOST\ stars interior to the Sun, LAMOST\ has observed more stars at $R$ beyond the Sun.
Consequentially, \emph{Gaia}{} and LAMOST{} together provide a better kinematic picture of the outer disk than \emph{Gaia}{} alone.
What's more, LAMOST{} spectra provide metallicities and chemical abundances.
We use distance estimates from \citet{bailer-jonesEstimatingDistancesParallaxes2018}, which used a Galactic prior together with \emph{Gaia}\ parallax to obtain distance posteriors for stars from both catalogs.

We used \texttt{galpy} \citep{bovyGalpyPythonLibrary2015} to calculate actions for each star with the St\"{a}ckel fudge \citep{binneyActionsAxisymmetricPotentials2012, bovyDirectDynamicalMeasurement2013} in the axisymmetric \texttt{MWPotential2014} model \citep{bovyGalpyPythonLibrary2015}.
We take the solar Galactocentric radius to be $R_0 = 8~\ensuremath{\mathrm{kpc}}$.
While kinematic uncertainties propagate to actions, they are small enough not to obscure the chemodynamical signatures we investigate in this paper.
\citet[Appendix D]{wheelerAbundancesMilkyWay2020a} show mean action uncertainties as a function of Galactocentric radius, $R$, for \emph{Gaia}{} DR2 and LAMOST{} DR 4, which have RV uncertainties very similar to \emph{Gaia}{} EDR3 and LAMOST{} DR 5.

\subsection{The MW disk as seen by LAMOST{} and \emph{Gaia}{}} \label{sec:dataoverview}
\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{lamost_kinematics.pdf}
    \caption{The LAMOST{} $J_\phi$--$J_R${} and $R$--$v_\phi${} planes in stellar density (top row; $\sim10^6$ stars), fraction of inwards-moving stars (second row; $\sim10^6$ stars), mean [Fe/H] (third row; $\sim10^5$ stars) and mean [Mg/Fe] (bottom row; $\sim10^5$ stars).
    The OLR ARLs for the three pattern speeds we consider are overplotted on the $J_\phi$--$J_R${} plane, and contours of constant $J_\phi$ corresponding the circular OLR orbits for the same pattern speeds are overplotted on the $R$--$v_\phi${} plane.
    The top four panels contain $~800,000$ stars and the bottom four contain $~95,000$, because we made additional cuts to mitigate abundance systematics.
    We use fewer stars when plotting metallicities or abundances because we restrict our sample to a small part of $\log(g)$--$T_\mathrm{eff}$ space to minimize systematics.}
    \label{fig:lamost_kinematics}
\end{figure*}

Figure \ref{fig:lamost_kinematics} shows the \emph{Gaia}{} + LAMOST{} $R$--$v_\phi${} and $J_\phi$--$J_R${} planes in stellar density, fraction of inwards-moving stars, mean [Fe/H] and mean [Mg/Fe], which is taken from \citet{wheelerAbundancesMilkyWay2020a}, who estimated detailed abundances for LAMOST{} DR4.
Note that [Fe/H] and [Mg/Fe] increase and decrease, respectively, with increasing $J_\phi$, $J_R$, $R$, and $v_\phi$
While we make use of [Fe/H] only in the remainder of this paper, we note that the results presented here can in principle be generalized to other abundances.
The ARLs for the OLR of $\ensuremath{\Omega_\text{p}} = 33.5~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$, $39~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$, and $51~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$ are plotted for orientation. In the \mbox{$R$--$v_\phi${}}
plane, contours of constant angular momentum are overplotted, corresponding to the values of $J_\phi$ on these OLR ARLs at $J_R = 0$.
These pattern speeds, used throughout the paper, correspond to a \emph{fast bar}{} whose OLR is associated with Hercules ($51~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$), an \emph{intermediate bar}{} ($39~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}})$, and a \emph{slow bar}{} ($33.5~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$).
The \emph{intermediate bar}{} and \emph{slow bar}{} OLR ARLs align with the ``Sirius'' and ``hat'' ridges, respectively, in the $J_\phi$ -- $J_R$ plane.
The \emph{fast bar}{} OLR ARL is slightly to the left of the inward-moving ridge that contains the "Horn" stars, and to the right of the outward-moving ``Hercules'' ridge with which the OLR of a rapidly rotating bar is often associated.
The exact values of the \emph{slow bar}{} and \emph{fast bar}{} pattern speeds are chosen so that their OLR ARLs align with transitions between net inwards and outwards movement with increasing $J_\phi$, as proposed by \citet{trickIdentifyingResonancesGalactic2021}.

In the $R$--$v_\phi${} plane, the ridges identified  with \emph{Gaia}{} \citep{kawataRadialDistributionStellar2018, gaiacollaborationGaiaEarlyData2021} and attributed variously to the bar, spiral arms, the Sagittarius dwarf galaxy, or a combination thereof \citep{antojaDynamicallyYoungPerturbed2018, khannaGALAHSurveyGaia2019, bland-hawthornGALAHSurveyGaia2019, fragkoudiChemodynamicsBarredGalaxies2019, fragkoudiRidgesUndulationsStreams2019a, laporteFootprintsSagittariusDwarf2019} are clearly visible.
The largest of these can be seen extending to a larger Galactocentric radius, $R$, than with \emph{Gaia}{} data alone.

\section{Simulations} \label{sec:sims}
To better understand the connection between bar resonance and chemistry in action space, we use test particle simulations with the same pattern speeds introduced in section \ref{sec:dataoverview} ($\ensuremath{\Omega_\text{p}} = 33.5~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$, $39~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$, and $51~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$). The setup of the simulations is analogous to those used by  \citet{trickIdentifyingResonancesGalactic2020a} and \citet{trickIdentifyingResonancesGalactic2021}, starting with an axisymmetric disk \citep{binneyModelsOurGalaxy2011} of massless particles, followed by integrating stellar orbits in an analytic MW potential model \citep{bovyGalpyPythonLibrary2015} that slowly introduces a bar perturbation \citep{dehnenEffectOuterLindblad2000, monariEffectsBarspiralCoupling2016}. The boxy bar model has $m=2$ and $m=4$ components \citep{huntOuterLindbladResonance2018a} with strengths $\alpha_{m=2} = 0.01$ and weak $\alpha_{m=4} = -0.0005$.
Orbits are integrated for 50 bar periods and the simulation snapshots at 20, 30, 40, and 50 bar periods are stacked to increase the number of particles to $4\times10^7$.

We assign metallicity values to test particles based on their positions in the intial disk, with a metallicity decreasing with both Galactocentric cylindrical radius $R$, and height from the midplane, $|z|$.
Each particle was assigned an iron abundance according to
\begin{equation}
    \mathrm{[Fe/H]} = -0.09~\left(\frac{R}{\ensuremath{\mathrm{kpc}}} - 6\right) + 0.2 - 0.21 \frac{|z|}{\ensuremath{\mathrm{kpc}}} + \varepsilon \quad ,
\end{equation}
where $\varepsilon$ is a random Gaussian perturbation with standard distribution 0.1.
The $R$ and $z$ dependence of this relation are based on the trends observed by \citet{haydenChemicalCartographyAPOGEE2014} in the low-alpha disk.
We note that the qualitative results of this work do not depend on the details of how metallicities are assigned, so long as the dominant trend is decreasing metallicity with Galactocentric radius.

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

\subsection{Metallicity signatures of bar resonances in action space} \label{sec:explanation}
\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{irene_explanation.pdf}
    \caption{The metallicity signatures at the bar resonances in the \emph{intermediate bar}{} test particle simulation.
    \textbf{A and B:} mean metallicity in the meridional plane for the axisymmetric and barred test particle simulations, respectively.
    \textbf{C and D:} number density in the $J_\phi$--$J_R${} plane for the axisymmetric and barred test particle simulations, respectively.
    \textbf{E and F:} mean [Fe/H] in the $J_\phi$--$J_R${} plane for the axisymmetric and barred test particle simulations.
    \textbf{G:} mean [Fe/H], in bins of $J_\phi$ and $J_R$, for the axisymmetric (dashed) and \emph{intermediate bar}{} (solid) test particle simulations.
    The CR resonance flattens the mean-metallicity trends, while the higher-order resonances (especially the OLR) create wave-crest signatures.
    \textbf{H:} differences between the above: the difference between mean [Fe/H] of each $J_R$ bin and the lowest $J_R$ bin.
    Error bars in the bottom two panels show the standard error in each bin.
    Except at the largest values of $J_R$ and $J_\phi$, the standard errors are too small to be visible, indicating that the trends are robust.
    The colored bands show the range of $J_\phi$ values each ARL takes on below $160~\ensuremath{\mathrm{kpc~km~s^{-1}}}$.
    }
    \label{fig:irene_explanation}
\end{figure*}

While bar resonances can change $J_\phi$ and $J_R$, they can not change a star's atmospheric metallicity, which remains very-nearly constant over a star's lifetime.
As discussed in Section \ref{sec:background}, actions oscillate in specific proportions at resonances, so kinematically distinguishing between resonances in observational data is possible in principle.
Stellar metallicities, however, provide an orthogonal source of information that makes this task much easier.
Figure \ref{fig:irene_explanation} demonstrates how bar resonances lead to signatures in $J_\phi$--[Fe/H] trends at different $J_R$.
The left column shows test particles evolved in an axisymmetric potential and the right shows particles evolved in the barred potential discussed in Section \ref{sec:sims}.
Panels A and B show the $R$--$z$ plane in metallicity, and panels C-F show the $J_\phi$--$J_R${} plane in both metallicity and density.
The bottom two panels show the [Fe/H] trends as a function of $J_\phi$, in bins of $J_R$ (panel G shows absolute metallicities, and panel H shows differences with respect to the smallest $J_R$ bin).
The error bars in the bottom two panels show the standard error, the scatter in metallicity over the square root of number of stars in each bin.
Except at the largest values of $J_R$ and $J_\phi$, the standard errors are too small to be visible, indicating that the trends are not due to sampling errors.
The colored bands in panels G and H show the range of $J_\phi$ values each ARL takes on below $160~\ensuremath{\mathrm{kpc~km~s^{-1}}}$.
The $J_R$ bin boundaries used in panels G and H are shown as horizontal lines in panels C-F.

Because stars in corotation with the bar oscillate strongly in $J_\phi$ without changing coherently in $J_R$  (Equation \ref{eq:jjlm}), and density changes slowly with $J_\phi$, the effect of the corotation resonance is difficult to see in stellar density in the $J_\phi$--$J_R${} plane.
Contrasting the mean [Fe/H] around the CR ARL for the barred and unbarred simulations reveals that the metallicity gradient becomes shallower when the bar causes stars to librate symmetrically in $J_\phi$, washing out the initial metallicity gradient.
This flattening is easily visible in panel G, where the metallicity gradient is visibly flattened.

At the other resonances (OLR, 1:1, and 1:4), $J_R$ changes in lockstep with $J_\phi$ (equation \ref{eq:jjlm}).
Because of the strong density gradient in $J_R$ (and weaker gradient in $J_\phi$), more stars are displaced from near-circular, low-$J_R$ orbits to eccentric, high-$J_R$ orbits than vice versa, creating a density ridge to the right of the corresponding ARL (panel D).
Below approximately $J_R = 50~\ensuremath{\mathrm{kpc~km~s^{-1}}}$, the metallicity contours to the right of the OLR ARL are more vertical in the barred simulation because stars on circular orbits have moved upward (and slightly to the right) in the $J_\phi$--$J_R${} plane, shifting the mean metallicity up at the location of the overdensity ridge.
In panels G and H, the chemical trends around the OLR are most easily identifiable.
For near-circular orbits ($0 < J_R~[\text{kpc km s}^{-1}] < 15$) in the barred potential, the mean metallicity drops only slightly below that in the unbarred potential.
This is because of the small number of lower-metallicity stars scattered from larger $J_\phi$ and $J_R$ to more circular orbits.
In contrast, among the more eccentric stars, the size of the deviation from the overall trend increases with $J_R$, with trends rising above that of the unbarred potential to form a ``wave-crest'' in the $J_\phi$-[Fe/H] plane across bins of $J_R$.
Like the OLR, the 1:1 and 1:4 resonances create metallicity wave-crests, but they are weaker because of the weaker Fourier $m = 4$ bar component, and the 1:1 comprising stars far beyond the bar.

\begin{figure}
    \centering
    \includegraphics[width=0.48\textwidth]{irene_comparison.pdf}
    \caption{Mean [Fe/H] as a function of $J_\phi$ in bins (same as Figures \ref{fig:irene_explanation} and \ref{fig:barstrength}) of $J_R$ for particles evolved in all three simulations.
    Error bars show the standard error.
    The flattening and wave-crest signatures are not sensitive to pattern speed.
    The vertical bands show the location of ARLs, as in Figure \ref{fig:irene_explanation}.
    }
    \label{fig:irene_comparison}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=0.45\textwidth]{barstrength.pdf}
    \caption{Mean [Fe/H] trends in $J_\phi$ and $J_R$ for two test particle simulations with different bar strengths, but the same pattern speed ($\ensuremath{\Omega_\text{p}} = 33.5~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$).
    Error bars show the standard error.
    Because the stronger bar traps more stars on resonant orbits, the metallicity signatures (at $\sim1500~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ and $\sim 2200~\ensuremath{\mathrm{kpc~km~s^{-1}}}$) cover a larger range in $J_\phi$, too.
    }
    \label{fig:barstrength}
\end{figure}

The wave-crest and flattening signatures at OLR and CR, respectively, in Figure \ref{fig:irene_explanation} do not change with pattern speed.
Figure \ref{fig:irene_comparison} shows the metallicity trends for particles evolved in all three simulations.
While the value of $J_\phi$ at which the resonances occur changes, the chemical signature of the resonances does not.
They do change with bar strength, however.
As the bar strength increases, the region of trapped orbits around the ARL becomes larger (c.f. \citealt{binneyOrbitalToriNonaxisymmetric2018}).
Figure \ref{fig:barstrength} shows the flattening and wave-crest for the \emph{slow bar}{} simulation, and for stars evolved in the same potential but with a bar of twice the strength ($\alpha_{m=2} = 0.02$, $\alpha_{m=4} = -0.001$).
The flattening in [Fe/H] at CR as a function of $J_\phi$ extends across a larger range of $J_\phi$, and the wave-crest at the OLR and 1:1 resonance become more extreme, with the mean metallicity for high-$J_R$ stars exceeding that of those on circular orbits in the resonance zone.

\subsection{Action-metallicity signatures in the LAMOST data}

\begin{figure*}
    \centering
    \includegraphics[width=0.85\textwidth]{lamostirene.pdf}
    \caption{Mean [Fe/H] as a function of $J_\phi$ in bins of $J_R$ for LAMOST{}.
    The errorbars show the standard error on the mean.
    There are not enough stars with $J_R > 60~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ to plot trends.
    Grey vertical bands mark the approximate $J_\phi$ of known moving groups for orientation.
    Gray dashed lines mark the $J_\phi$ values of circular orbits with $R$ at the radius where the solar azimuth intersects hypothesized spiral arms (taken from \citealp{reidTrigonometricParallaxesHigh2014}).
    Observational data is not yet plentiful enough to clearly identify or rule out the resonance signatures described in section \ref{sec:explanation}, but the flattening around $1400~\ensuremath{\mathrm{kpc~km~s^{-1}}} < J_\phi < 1700 ~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ and the elbow at $J_\phi \approx 220~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ are suggestive of a slow bar.
}
    \label{fig:lamost_irene}
\end{figure*}

Figure \ref{fig:lamost_irene} shows mean [Fe/H] as a function of $J_\phi$ and $J_R$, the diagnostic introduced in section \ref{sec:explanation}, drawn with the observational data introduced in Section \ref{sec:data}.
The three panels show ARL zones corresponding to the three pattern speeds used in the test particle simulations.
The limitations of available data (the number of stars observed, their spatial coverage, and uncertainties and biases in their metallicities) make it difficult to clearly identify either the flattening or wave-crest signatures.
Only for $\ensuremath{\Omega_\text{p}} = 33.5~\ensuremath{\mathrm{km~s^{-1}~kpc^{-1}}}$ are both the CR and the OLR region populated with data, although this is sensitive to the rotation curve of the approximate axisymmetric potential used to calculate actions.
Increasing incompleteness with distance from the Sun yields mean-[Fe/H] uncertainties large enough to obscure potential resonance signatures for $J_\phi \lesssim 1600~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ and $J_\phi \gtrsim 2700~\ensuremath{\mathrm{kpc~km~s^{-1}}}$, even though some data is present.
As we will discuss in section \ref{sec:sellection}, the azimuthal coverage of the LAMOST{} and \emph{Gaia}{} data also obscure a potential signature of bar resonances.

In the context of the above caveats, we note that the hint of a wave-crest is present in Figure \ref{fig:lamost_irene} around $J_\phi \approx 2200~\ensuremath{\mathrm{kpc~km~s^{-1}}}$, i.e. close to the Hat moving group.
There is a flattening in the mean [Fe/H] trend at $J_\phi \lesssim 1600$ (which corresponds to $R=7.5~\ensuremath{\mathrm{kpc}}$).
Similar trends have been observed before in the Milky Way \citep{haydenCHEMICALCARTOGRAPHYAPOGEE2015, haywoodPhylogenyMilkyWay2018, haywoodRevisitingLongstandingPuzzles2019} and in other galaxies \citep{stottRelationshipSpecificStar2014, leethochawalitKeckSurveyGravitationallyLensed2016}, and have been largely attributed to well-mixed gas, although \citet{haydenCHEMICALCARTOGRAPHYAPOGEE2015} states that stellar migration due to the bar is the likely cause.
If the flattening is caused by stellar migration, rather than the birth properties of stars in the inner disk, it is consistent with the CR resonance of a slow (circa $33.5~\ensuremath{\mathrm{kpc~km~s^{-1}}}$) bar.

The dependence of mean [Fe/H] on $J_R$ differs strongly across $J_\phi$.
For $J_\phi \lesssim 2000~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ (at least until $J_\phi \approx 1600~\ensuremath{\mathrm{kpc~km~s^{-1}}}$, when the uncertainties become large), stars on higher-eccentricity orbits have lower [Fe/H].
For $J_\phi \gtrsim 2000~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ the dependence is much weaker.
This effect is not a direct consequence of the dependence of [Fe/H] on height from the disk, $|z|$, surface gravity, $\log g$, or effective temperature, $T_\mathrm{eff}$.
It also does not appear to be caused by ``contamination'' from the high-$\alpha$ disk, since removing stars with large [Mg/Fe] (per \citealp{wheelerAbundancesMilkyWay2020a}) does not have any effect.
Additionally, the dependence of mean [Fe/H] on $J_R$ exhibits the same behavior when Figure \ref{fig:lamost_irene} is made with APOGEE \citep{majewskiApachePointObservatory2017} DR16 \citep{ahumada16thDataRelease2020}, rather than LAMOST{} data.
We conclude that it is likely physical, rather than an artifact of the observational data or our analysis.

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

\subsection{The influence of the spatial selection functions on the metallicity and actions}
\label{sec:sellection}
\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{simple_sellections.pdf}
    \caption{ The location of observed stars (i.e. the spatial selection function) has a strong impact on the flattening and wave-crest signatures.
    Here, resonance signatures as exhibited by stars in different azimuthal regions of the disk in the \emph{intermediate bar}{} simulation are plotted.
    $J_R$ bins above $60~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ are not plotted because of the lack of sufficient data.
    Each row shows stars within a cylinder centered at the solar Galactocentric radius at different azimuths: exactly along the minor axis of the bar (top), in the position of the Sun (middle rows), and exactly along the bar's major axis (bottom).
    The left column shows number density in the $X$--$Y$ plane, i.e. the footprint of each mock data set in the disk.
    The white line marks the orientation of the bar, and the white star marks the location of the Sun.
    The right column shows metallicity trends in $J_\phi$ and $J_R$ for each region.
    In row 3, only stars with azimuth farther from the bar azimuth than the Sun are used.
    The CR flattening and the OLR wave-crest are much more prominent in stars anti-aligned with the bar, but could be seen in a large volume of local data by plotting only stars farther from the bar's azimuth than the Sun (row 3).
    }
    \label{fig:simple_sellections}
\end{figure*}

The bar and spiral arms have been shown to lead to a nonaxisymmetric metallicity distribution (e.g. \citealp{dimatteoSignaturesRadialMigration2013, grandSpiralinducedVelocityMetallicity2016, khoperskovStellarMetallicityVariations2018, fragkoudiDiscOriginMilky2018}), meaning that the spatial location of the observational data with respect to the bar has a significant impact on both the wave-crest and flattening signatures.
In contrast to previous Figures, which use stars at all azimuths, Figure \ref{fig:simple_sellections} shows mean [Fe/H] trends in $J_\phi$ and $J_R$ using only stars within cylinders centered at different points in the disk for the \emph{intermediate bar}{} test particle simulation, demonstrating that stars with azimuth nearer to the bar's minor axis show the resonance signature much more prominently.\footnote{Particles with positive $X$ are rotated $180^\circ$ to the Sun's side of the Galaxy to increase the number available to plot.}
All cylinders are centered on points 8 kpc from the center of the disk, the approximate Galactocentric radius of the Sun.
The first row, which plots stars centered on a point on the bar's minor axis (i.e. with $\phi = \phi_\odot - 75^\circ$, taking the bar's pitch angle to be $25^\circ$), exhibits resonance signatures much stronger than the others.
For these stars, the flattening at CR turns sharply on and off for each $J_R$ bin, and the OLR wave-crest is very strong, with mean [Fe/H] dependence on $J_R$ fully inverting at $J_\phi \approx 2250~\ensuremath{\mathrm{kpc~km~s^{-1}}}$.
For survey volumes centered on the Sun or aligned with the bar's major axis (rows 2 and 4 in Figure \ref{fig:simple_sellections}), the CR flattening and OLR wave-crest are attenuated and nearly absent, respectively.
But if only the stars within 3 kpc of the Sun which are farther from the bar azimuth than the Sun are plotted, both signatures become much more prominent (Figure \ref{fig:simple_sellections} row 3), demonstrating that a sample in the ``extended solar neighborhood'' can be used to uncover these features.

\begin{figure}
    \centering
    \includegraphics[width=0.45\textwidth]{flatteningsig.pdf}
    \caption{
    The ``banana-shaped'' orbits of stars trapped at CR spend little time near the bar's major axis, and many dwell exclusively near its minor axis, which explains the azimuthal sensitivity demonstrated in Figure \ref{fig:simple_sellections}.
    The relative slope of the $J_\phi$--[Fe/H] relation around CR with respect to the overall slope for stars with $J_R < 60~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ as a function of position in the disk for the \emph{intermediate bar}{} simulation.
    The black rectangle indicates the orientation of the bar.
    The orbits of two stars trapped by the CR resonance are overplotted (in the rotating frame).
}
    \label{fig:crmap}
\end{figure}
Figure \ref{fig:crmap} shows the degree of CR flattening as a function of position in the disk with two CR orbits plotted, demonstrating again the importance of the azimuth of observed stars and helping to reveal its cause.
It is colored by the slope of the $J_\phi$--[Fe/H] relation for stars roughly in the \emph{intermediate bar}{} CR region, with $1200 ~\ensuremath{\mathrm{kpc~km~s^{-1}}} < J_\phi < 1300~\ensuremath{\mathrm{kpc~km~s^{-1}}}$ and $J_R < 60~\ensuremath{\mathrm{kpc~km~s^{-1}}}$, minus the slope outside the CR zone (calculated with the stars in $1600~\ensuremath{\mathrm{kpc~km~s^{-1}}} < J_\phi < 1800~\ensuremath{\mathrm{kpc~km~s^{-1}}}$).
This figure shows, similarly to Figure \ref{fig:simple_sellections}, that the CR flattening is much stronger in stars around the bar's minor axis.\footnote{There is a weak asymmetry in the metallicity slope at CR around the bar's minor axis, at about $Y = 4~\ensuremath{\mathrm{kpc}}$, slightly ahead of the minor axis in Figure \ref{fig:crmap}. This is a phase-mixing relic in the simulation which depends on how stars with different initial phases and metallicities get scattered at CR.}
The two grey lines show the paths of two stars trapped by the CR resonance as they orbit over 3000 time steps.
The azimuthal dependence is a consequence of the ``banana'' shape of these orbits, which oscillate around Lagrange points 4 and 5 on the bar's minor axis.

\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{irene_selections.pdf}
    \caption{Mean [Fe/H] as a function of $J_\phi$ and $J_R$ for the \emph{intermediate bar}{} simulation with the LAMOST{}'s spatial selection function imposed.
    \textbf{top: }full LAMOST{} footprint.
    \textbf{bottom: }partial LAMOST{} footprint, with only stars with azimuth less than the Sun's.
    The flattening and wave-crest signatures at CR and the OLR, respectively, are extremely attenuated because stars are concentrated near the Sun.
    }
    \label{fig:lamost_selections}
\end{figure*}

We use a simple rejection sampling scheme to simulate the LAMOST{} spatial selection function in detail and understand why current data is inadequate to reveal the signatures explored in this work.
We approximate the spatial distribution of the test particles and LAMOST{} stars, $p_\mathrm{sim}(\mathbf{r})$ and $p_\mathrm{LAMOST}(\mathbf{r})$, where $\mathbf{r}$ is 3D position, by counting the fraction of stars in each bin in a fine grid\footnote{Bin sizes are 0.5 kpc in the $X$ and $Y$ dimensions, and 0.1 kpc in the $z$ dimension}, then interpolating with a cubic spline.
We then include each test particle in the subset for comparison with probability proportional to the ratio of $p_\mathrm{sim}(\mathbf{r})/p_\mathrm{LAMOST}(\mathbf{r})$.
This reduces the number of particles from $4\times 10^7$ to about $1.6 \times 10^5$, but allows a more ``apples to apples'' comparison between simulation and data.
Figure \ref{fig:lamost_selections} shows the mean [Fe/H] trends in action space for the \emph{intermediate bar}{} simulation with the observational spatial footprint imposed.
(The results are similar for the \emph{slow bar}{} and \emph{fast bar}{} simulations.)
Both the wave-crest and flattening are attenuated and distorted by the limited azimuthal coverage.
The first row uses the full observational footprint, and the second row uses the same cut as Figure \ref{fig:simple_sellections} row 3, keeping only stars with azimuth closer to the bar's minor axis than the Sun.
Both selections are too concentrated near the Sun to show the signatures clearly.
While LAMOST{} and other current datasets don't have the spatial coverage to look for resonance signatures in stars further away from the bar's major axis, in the near-future metallicities from the \emph{Gaia}{} RV spectrograph or Sloan-V \citep{kollmeierSDSSVPioneeringPanoptic2017} will likely make such an analysis possible.

\section{Conclusions} \label{sec:conclusions}
We investigate the effect of bar resonances on the metallicity distribution in the Milky Way's thin disk as a function of the stars' orbital actions, $J_\phi$ and $J_R$.
We use test particle simulations of a stellar disk in a Milky-Way-like gravitational potential with a simple rotating bar to identify distinct signatures: The corotation resonance leads to a flattening of the metallicity gradient, and higher-order resonances, especially the Outer Lindblad resonance; this creates a ``wave-crest'' in the mean [Fe/H] as a function of $J_\phi$ binned by $J_R$.
We confirm that these signatures do not change qualitatively with pattern speed or strength, although the strength of the signal varies with bar strength.
We demonstrate that a survey's selection function can strongly affect the appearance of these signatures.

We search for these resonant metallicity-vs.-action features in stars using metallicities and RVs from LAMOST{} DR 5 and parallaxes, proper motions, and supplementary RVs from \emph{Gaia}{} EDR3.
While distinguishing signatures of bar and spiral resonances remains difficult, the diagnostics discussed here can identify both the OLR and CR resonance at once.
We find weak evidence for a slow bar associated with the ``hat'' moving group, but conclude that present data does not allow us yet to unambiguously identify these signatures.
Interpreting observational data is made more difficult, not only by the complexities of the Galaxy not present in our simplified test particle model, but also because current surveys provide 6-D kinematics and metallicities only for stars in a limited region of the Galactic disk.
In particular, we show that the strength of the flattening and wave-crest signatures depends on the Galactocentric azimuth.
The strongest signature is found at an azimuth along the bar's minor axis, while along the bar's major axis the resonant signature in the metallicity almost vanishes.
Consequently, our observing location within the Galactic disk, $\sim 25^\circ$ behind the bar, is not optimal, but observations of more stars with Galactocentric azimuth far from the major-axis of the bar, which near-future data will deliver, can remedy this.

There are several promising directions for future progress on chemo-dynamically identifying bar resonances.
In this paper, we have used a fairly simple galaxy model as basis for the comparison to the data. More complex models may yield modified predictions.
For example, a bar with significant deceleration will trap stars with a different distribution of orbits \citep{chibaResonanceSweepingDecelerating2019}, and \citet{chibaTreeringStructureGalactic2021} show that metallicity should decrease from the center of the corotation resonance to its boundary.
$N$-body models with self-consistent bars could also provide a richer picture, including the possibly confounding effects spiral arms, which impact metallicity distributions and can overlap with bar resonances.
Stellar ages and chemical abundances beyond [Fe/H] provide additional clues to a star's birth location and, given a better understanding of the Galaxy's chemical evolution, can doubtlessly further constrain birth radius.
On the other hand, if the bar resonances can be conclusively identified by other means, their chemical abundances inform us on the star formation history of the disk.
Sloan V and \emph{Gaia}{}'s future data releases, which will increase the azimuthal coverage of suitable data, will likely allow us to pinpoint the pattern speed of the bar and shed light on the Galaxy's dynamical structure.

\software{galpy \citep{bovyGalpyPythonLibrary2015}, Matplotlib \citep{hunterMatplotlib2DGraphics2007}}

\section*{Acknowledgments}
The authors would like to thank Jason Hunt, Tomer Yavetz, Kathryn Johnston, and the Milky Way stars group at Columbia for useful discussion and suggestions.

AJW is supported by the National Science Foundation Graduate Research Fellowship under Grant No. 1644869. MKN is in part supported by a Sloan Research Fellowship.

Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences.

This work has made use of data from the European Space Agency (ESA) mission {\it Gaia} (\url{https://www.cosmos.esa.int/gaia}), processed by the {\it Gaia}
Data Processing and Analysis Consortium (DPAC, \url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the {\it Gaia} Multilateral Agreement.

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Pursuant to Section 13 or 15(d)
Date of Report (date of earliest event reported): April 14, 2021
SOLENO THERAPEUTICS, INC.
File No.)
203 Redwood Shores Pkwy, Suite 500
Written communications pursuant to Rule 425 under the Securities Act (17 CFR 230.425)
Soliciting material pursuant to Rule 14a-12 under the Exchange Act (17 CFR 240.14a-12)
Pre-commencement communications pursuant to Rule 14d-2(b) under the Exchange Act (17 CFR 240.14d-2(b))
Pre-commencement communications pursuant to Rule 13e-4(c) under the Exchange Act (17 CFR 240.13e-4(c))
Name of each exchange
on which registered
Common Stock, $0.001 par value SLNO NASDAQ
Indicate by check mark whether the registrant is an emerging growth company as defined in Rule 405 of the Securities Act of 1933 (§ 230.405 of this chapter) or Rule 12b-2 of the Securities Exchange Act of 1934 (§ 240.12b-2 of this chapter).
ITEM 8.01
On April 14, 2021, Soleno Therapeutics, Inc. (the "Company") issued a press release announcing that Anish Bhatnagar, M.D., the Company's Chief Executive Officer, participated in a Prader-Willi Syndrome ("PWS") Town Hall meeting hosted by the PWS Community. The Town Hall was held on Wednesday, April 14, 2021 and discussed the use of Diazoxide Choline Extended-Release Tablets ("DCCR") in PWS. The event featured speakers from the PWS community who provided insights into the challenges of living with PWS as well as patient and caregiver perspectives on DCCR treatment. As part of the meeting Dr. Bhatnagar's spoke and his remarks highlighted the unmet medical needs facing PWS patients, the company's ongoing commitment to obtaining regulatory approval for DCCR and an outline of the necessary steps to obtain regulatory approval of DCCR. The remarks have been published as an open letter to the PWS community.
A copy of the open letter to the PWS community is attached hereto as Exhibit 99.1 and is incorporated herein by reference.
A copy of the press release is attached hereto as Exhibit 99.2 and is incorporated herein by reference.
Financial Statements and Exhibits
(d) Exhibits
99.1 Open letter to the PWS community dated April 14, 2021.
99.2 Press release issued by Soleno Therapeutics, Inc. dated April 14, 2021.
/s/ Anish Bhatnagar
Anish Bhatnagar