January 20-26 is National Non-Smoking Week!
Did you know most tobacco users want to quit? Or that smoking tobacco is the leading cause of preventable disease, disability, and death? Yikes! This week, let's work on helping to prevent young people from starting to smoke or chew tobacco and helping the tobacco users in your life quit so we can protect everyone from the harms of second- and third-hand smoke.
There are free provincial resources to help people quit – they can quit for a day and work towards a long term quit plan! Interested? Here's three quitting resources you should check out now.
QuitNow: get free counselling and support by visiting QuitNow or calling 1 877-455-2233. They even text! Text QUITNOW to 654321.
Free quitting products through the BC Smoking Cessation Program: all British Columbians can access FREE Nicotine patches, gum, lozenges, or inhalers through the BC Smoking Cessation Program to help reduce cravings while trying to quit. Talk to your pharmacist. You may be eligible for help to buy smoking cessation medications such as Varenicline (Champix) or Bupropion (Zyban).
Make a plan and find a friend: if you smoke, plan to quit; if you don't smoke, help a tobacco user quit!
In this story, as in most public health messages, "tobacco use" refers to the use of commercial tobacco products like cigarettes and chewing tobacco as opposed to traditional uses of tobacco. Northern Health supports the cultural and ceremonial uses of tobacco and recognizes that the benefits of traditional uses can outweigh the potential harms.
The City of Prince George promotes a healthy environment for all to enjoy. Two years ago on May 1, 2016 the city council adopted a bylaw to regulate smoking and vaping in outdoor areas and joined 68 other municipalities in BC who have a bylaw limiting where you can use tobacco in outdoor spaces. Smoking or vaping is prohibited within 25 metres of any outdoor sport facility or playground or other places where the public gather.
The bylaw restricts the smoking of cigarettes, cigars, pipes, hookah pipes, or other lighted smoking equipment that burns tobacco or other weed or substance. This means that the smoking of cannabis will also be restricted.
On May 1, 2016 the Prince George city council adopted a bylaw to regulate smoking and vaping in outdoor areas.
Exposure to second hand smoke from burning tobacco products and other substances causes disease and premature death among non-smokers and this step has reduced the harmful effects of tobacco smoke for the people of Prince George. Exposure to vapour has been linked to some health risks although vaping is considered to be safer than smoking tobacco products. Children are particularly vulnerable to second hand smoke and vapour as they breathe faster and are exposed to even more smoke and vapour.
The bylaw also helps reduce the amount of litter from butts and discarded cigarette packaging. The filters do not biodegrade and litter the ground until swept up. As we enter a potentially hot, dry summer, this bylaw can also reduce the risk of fire from discarded matches and tobacco products.
Supportive smoke free environments help people who have quit using tobacco stay quit and also encourage tobacco users to quit. If your city or town does not have a bylaw to protect everyone from second hand smoke and vape, perhaps you would consider working with your local government to create one.
Are you wishing that you never started? Do you hope that your kids never start? You are probably planning to quit someday. Why not make it today? Have a look at these nine reasons to quit and feel free to add your own.
My health will improve within eight hours of my last cigarette.
I can stop worrying about how smoking is hurting my health. I will lower my chances of getting cancer, heart disease, lung disease, and other disabling diseases. I will also look younger.
Winter is coming. I won't have to go outside in nasty weather to smoke or buy cigarettes etc.
I will save money! I will have more money for Christmas and other fun stuff.
My clothes, house, or car won't smell like smoke.
I won't have to live with the constant cravings to smoke or chew once I have quit.
I will feel more in control of my life. Smoking isn't cool anymore.
I will no longer expose my friends and family to the harmful effects of second hand smoke.
I will help prevent my kids from getting addicted to tobacco.
The Provincial Smoking Cessation Program helps eligible BC residents who wish to stop smoking, or using other tobacco products quit, by covering the cost of nicotine replacement therapy (NRT) products, and helps with the cost of specific smoking cessation prescription drugs. Visit your local pharmacy to pick up your first month of patches, gum, inhalers, or lozenges. There are twelve weeks left in 2017 and you can access another twelve weeks of NRT in January of 2018.
You can also access counselling by phone, email or text. Visit QuitNow or call 1-877-455-2233 for support from QuitNow services.
Northern Health supports the cultural and ceremonial uses of tobacco and recognizes that the benefits of traditional tobacco use can outweigh the potential harms.
I grew up in southern Ontario near the "tobacco belt" of Norfolk and Elgin counties. I remember the green buildings with red roofs throughout the area: the kilns where tobacco was hung to dry. Many prosperous farms existed in this sandy- and silt-loam soil.
In recent years, the production of tobacco in this area has decreased thanks to the decline of tobacco use* in Canada and the pressure on farmers to stop producing. Farmers are now growing products such as lavender, peanuts, and ginseng and some have started wineries, poultry farms, and apiaries.
What does tobacco production look like on the global stage?
This year, for World No Tobacco Day, the World Health Organization has chosen the theme: "Tobacco – A Threat to Development." How is tobacco a threat to development?
Worldwide, the production of tobacco requires large amounts of pesticides and fertilizer that can pollute water supplies. Like in my home counties, the land used for tobacco could grow food instead of tobacco, a product that kills half of those who use it. Without protective clothing that many of us take for granted, workers are exposed to nicotine and harmful pesticides labouring in tobacco fields. In many countries, these labourers are children.
Locally, regionally, and nationally, we need to develop strategies to prioritize tobacco control and reduction. Tobacco use remains the leading cause of preventable death in both Canada and worldwide and kills half of the people who use it.
Tobacco reduction works in communities to prevent the initiation of smoking among young people, protects the public from second-hand smoke in community settings, and increases tobacco cessation and tobacco reduction efforts within primary care settings, while recognizing and valuing traditional tobacco use through cultural and ceremonial use.
World No Tobacco Day reminds us that we can work together to prevent children from starting to use tobacco, protect everyone from the harmful effects of second-hand smoke in both indoor and outdoor spaces, and encourage tobacco users to stop using these products.
Do you know someone who smokes? Encourage them to check out QuitNow.ca and access free nicotine patches, gum, lozenges, or inhalers through the BC Smoking Cessation Program.
*In this story, as in most public health messages, "tobacco use" refers to the use of commercial tobacco products like cigarettes and chewing tobacco as opposed to traditional uses of tobacco.
What are your reasons to quit?
Do you smoke cigarettes or chew tobacco? Everyone knows that smoking cigarettes or chewing tobacco is bad for your health. Are you wishing that you never started? Do you hope that your kids never start?
You are probably planning to quit someday. Why not make it today!
I can stop worrying about how smoking is hurting my health. I will lower my chances of getting cancer, heart disease, lung disease and other disabling diseases. I will also look younger.
It's cold outside. I won't have to go outside in nasty weather to smoke or buy cigarettes.
My clothes, house and car won't smell like smoke.
There are many resources available for you to quit smoking today!
I will help prevent my kids from getting addicted to cigarettes or chewing tobacco.
Want more information about quitting smoking?
Visit quitnow.ca or call HealthLink 8-1-1 for free self-directed programs and many helpful tools and resources. Get free counselling by phone, text or email.
You can access free nicotine patches, gum, lozenges or inhalers through the BC Smoking Cessation Program by visiting your pharmacist. You may be eligible for prescription smoking cessation drugs at reduced cost.
Quitting smoking or chewing tobacco is the best thing you can do for your health.
Quitting is hard, what's your story? Wrap-up and Fitbit winner!
Since World No Tobacco Day (May 30) Northerners have been sharing their 'Quit Stories'. I'd like to share a few more of the stories that came in, but first, many congratulations out to Melanie in Fort St. John whose name was drawn in the story entry contest to win a Fitbit Activity Tracker. Congratulations Melanie!
If you really want something you will achieve it!
My brother has smoked for 36 years. Recently he had pneumonia and a collapsed lung. It was only then that he quit. He always wanted to, but said that he would go through such bad withdrawals that he would just start smoking again. A doctor he saw, told him that his lung capacity was only about 38%, and that he needed to quit right away. This scared him so badly, that he quit. The truth was that he was so sick, that he could not smoke, he could hardly breathe. Now he tells me it was the best thing he ever did for himself. It was just too bad that it took such an extreme situation for him to quit.
I moved to Terrace in 2008. After 10 years of smoking, and being an asthmatic, I had been hospitalized hundreds of times. Each time becoming more and more serious. When we moved I felt this would be a great time to quit, new town new me. It was incredibly hard. I never thought about the stress of a new town along with the cravings to smoke and at the time my partner was still smoking. I continued and was successful and then was able to encourage my partner who then quit in Dec of the same year. It's been 8 years now and we are both healthier and happier. The monies we saved from smoking we now use to go on holidays. We continued to move the money we were spending on cigarettes into an account we opened and labelled "holiday" it's amazing how much money we were spending without realizing it. This gave us a twofold benefit. We are healthier and we have holiday money which we were not previously making a priority.
Many more stories came in and I wish I could list them all, but space will allow me only to thank everyone who shared their quit story and entered the contest. We are all touched by tobacco use and it takes a lot of hard work and determination to quit –but it helps everyone around you when you do.
Do you want to quit? Speak with your health care provider and for information and free support to help you, visit QuitNow or call 1-877-455-2233. You can also ask your pharmacist how to access information and FREE nicotine patches, gum, lozenges or inhalers through the BC Smoking Cessation Program.
True-life quit stories – northerners going tobacco-free!
Quitting smoking is hard, what's your story?
The "Quit Story contest" deadline is this Friday (June 10th) and so far the submissions have been heartfelt and inspiring.
Before sharing these stories, I should note that your quit story can also involve your experience with the quit attempts of people in your life – we've all been touched by tobacco use through our family, friends and work. Many thanks to all who have entered the contest and shared their stories – perhaps these words can help support your decision, or that of someone in your life. You can share your story and enter the contest to win a Fitbit activity tracker until Friday – so keep those quit stories coming!
"I started smoking when I was 16 and quit when I was 40, wow, that's a lot of years. I sort of tried to quit everytime a new "program" came out; gum, patches, pills, etc. There was something about smoking that I liked though, not just the buzz it gave me but the time away from the kids, household chores, work, life. It was a time for me to zone out for a few minutes or to socialize with other smokers in the back parking lot. I tried to be a courteous smoker, always outside, away from doors and windows and I would justify my addiction by saying it's really the only bad habit I had. I had lost family members to lung cancer but always thought well, if that's what's gonna get me then so be it.
Call it an epiphany, or a light bulb moment, whatever… I sitting on my front step, taking a mom's time out when I realized that I didn't want to do it anymore, I didn't want to leave the kids in the house and hide out so I could have a smoke. That was it, I went to doctor, had a little cry, told him I wanted to try the new drug to quit, didn't hurt that I was also feeling depressed and needed the anti-depressant part too. I took the drug for 2 months then stopped because of the side effects. I told myself over and over again that I didn't want to go through all that again, I didn't want to hide, or disappoint or make excuses for my behaviour. I had two very smart children watching me as well, making sure I didn't slip. I tested myself once, after about 4 months, stupid thing to do and I don't recommend it! I took a drag off my friend's cigarette and was so dizzy and queasy that I couldn't take another drag, if I did, I would have been right back at it again. I never tested myself again. I always thought I would like to be one of those smokers that only smokes when they have a few drinks, but then I would be an alcoholic.
I'll share more stories before the end of the week – I'm excited to read all that come in. Sometimes these aren't easy stories to tell, thank you for your words.
The contest runs until Friday, the 10th, so enter today! You can win a Fitbit activity tracker to keep you on your toes!
Want to access online support and counselling as part of your plan to quit smoking this year? QuitNow has free services available to support you!
Today is the start of National Non Smoking Week! Many tobacco users use this opportunity to quit smoking. It often takes a few tries to successfully quit smoking. The more you are prepared, the more likely it is that you will succeed.
There are many reasons why people smoke, but 70% of tobacco users want to quit and many wish that they had never started. If you have tried to quit before, think about that experience and recognize what worked and also what made you relapse.
Nicotine is a very addictive substance and causes uncomfortable withdrawal when you go for a period of time without smoking. Smoking is also a learned behaviour that you may associate with certain feelings or activities. It may also be a social activity for some. The addiction is quite complex and unique to each individual.
Because of this, I recommend that you keep a diary of your smoking prior to quitting to identify your triggers and to help you change your behavior to reduce your smoking. Record what you were doing when you decided to smoke and why you feel you need one. You may even find that you reduce the amount you smoke prior to quitting.
Are you going to use nicotine replacement therapy or other medications? If so, check out the BC Smoking Cessation Program for free products.
Are you going to tell your friends to gain support or are you going to keep it to yourself?
Are you going to access online support and counselling through QuitNow services?
What is your measure of success? Have you completely quit or cut back? Are you still craving?
Quitting smoking is the best thing you can do for your health. You will feel better, have more money in your pocket and no longer have to worry about quitting!
The BC Smoking Cessation Program is now easier than ever to access. As of January 1, 2016, you can get 12 weeks of free nicotine replacement therapy products (including gum, patches, lozenges, and inhalers) just by visiting any pharmacy in the province. You may also qualify for assistance for other tobacco cessation medications. For more information, visit QuitNow.ca or call HealthLink (8-1-1).
Every day is a good day to quit smoking. Plan to make 2016 your smoke free year!


text:
Q: how to forward a fluentd log file? I have a file, which is written by fluentd as format: out_file.
Now I want to forward the content of this file to another fluentd-agent, with tag changed.
But the problem is: the file content will be wrapped again, for example:
the original line is:

2017-09-29T20:57:34+08:00   fluentd.test.follow {"from":"A","to":"B"}

and the new line will be:

2017-09-29 22:39:52 +0800 center.test: {"message":"{\"from\":\"A\",\"to\":\"B\"}"}

What SHOULD I do, so I can get the content like this?

2017-09-29T20:57:34+08:00   center.test {"from":"A","to":"B"}

A: Fluentd offers forwarding to another Fluentd process through a different plugin called out_forward. https://docs.fluentd.org/v0.12/articles/out_forward
In order to achieve the different structure of Fluentd you should use the record_reformer plugin that allows you to add fields or perform calculations on top of fields
https://docs.fluentd.org/v0.12/articles/filter_record_transformer

redpajama_set_name: RedPajamaStackExchange


text:
Game Review: The Pedestrian
moshfish February 11, 2022 February 27, 2022 Video Games
Version played: Xbox Series X in 2022
Both developed and published by Skookum Arts LLC, The Pedestrian is a side-scrolling (sort of) puzzle platformer originally released in 2020 for PC, but onto Xbox Series X two years later in 2022. Players control a stick figure man or woman as they move through signs which populate our real world. To progress, the doors on these signs need to be linked together and the physical location of the signs may need to be changed, as well a few gimmicks introduced later into the game's single player experience.
+ the art style is immediately charming, and every now and then you'll feel the need to stand still in a sign just to make it look like a real world location
+ the game introduces new mechanics as it goes, such as opening gates in the real world to rearrange the order of signs, or needing to run electricity through one sign. The game reached a fine balance between pre-planning and making connection decisions on the fly, which I found immensely satisfying
Your character begins as a simple shape on a whiteboard…
Connecting doorways will allow you to jump between signs.
The great outdoors (and an unused title image for this very review!)
– the whole game is very short, to the point where I worried that maybe I had accidentally skipped entire sections when travelling from one area to the next. The achievement list proves that not to be the case
– I'll be honest, I was really confused when I finished this. The story is barebones, if there is a story at all, and a fun little gameplay twist comes a bit too late in the game for my liking
> as is seemingly the norm with every puzzle game I review, there was but one puzzle that really stumped me, and once I figured it out I felt like a dumbo. Yes, I was misreading something super obvious
Should you play this game: Xbox Game Pass has been an absolute god send for these short puzzle games, and insofar as that goes then I enjoyed my time on this. But an AUD $30 price tag seems a bit steep for what it's offering. If you can play this for cheaper — or better still, essentially for free on Game Pass — then you will have a short but sweet time.
2022, 2d, game pass, Platformer, Puzzle, Review, side scroller, sign, skookum arts llc, the pedestrian, Video Game, xbox series x
Previous Game Review: Children of Morta
Next Wrestling Review: NXT 2.0 Vengeance Day (2022)

redpajama_set_name: RedPajamaCommonCrawl


I don't know if it's my mother's love of puzzling, my ability to solve the Rubik's cube in under 30 seconds, or just the need to avoid conversations with people on the light rail, but we're always looking for a new cool game to get sucked into.
Candy Crush, Two Dots, 2048 - all games that at times masterfully provide a temporary escape inside the depths of your brain - well, the left side at least. The trailer alone for Tiny Bubbles makes me feel better, calmer, less annoyed by all the prickly things poking at me during my busy day downtown.
This game reminds me of the best parts of Spore - an evolution game that starts in the steamy waters of early life - meets a puzzle game. So soothing like a hot spring with little minnows nibbling at your dead toe skin. Gross. Not like that at all.
Tiny Bubbles is made right here in Washington via Pine Street Code Works - an independent gaming company with just one full-time employee and a bunch of help from friends! Based on the accolades (below), this thing is going places. I got the duo responsible for this game on Skype to tell me about the demands of making your own game!
Make sure you check out Tiny Bubbles when you're at GE2 this weekend!


Cab Guru sends three types of notifications; booking, informational and promotional.
These are sent in the form of push notifications, SMS text messages and emails.
Booking notifications are sent when something significant happens to your booking. For example, we will send a notification when your booking is dispatched to a driver, and when they arrive at the pickup point.
Informational notifications may include updates on local transport issues.
From time to time we will send you relevant promotional offers as a valued customer of Cab Guru.
You can opt out of these notifications at any time by amending your notification settings, for more help on changing your notification settings click here.


text:
<?php

namespace Emtudo\Domains\Users\Repositories;

use Emtudo\Domains\Users\Contracts\UserRepository as Contract;
use Emtudo\Domains\Users\Queries\UserQueryFilter;
use Emtudo\Domains\Users\User;
use Emtudo\Support\Domain\Repositories\Repository;

class UserRepository extends Repository implements Contract
{
    protected $modelClass = User::class;
    protected $queryFilterClass = UserQueryFilter::class;

    public function setModelData($model, array $data)
    {
        parent::setModelData($model, $data);

        if (isset($data['password']) && !empty($data['password'])) {
            $model->password = $data['password'];
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
Spirit of Place
Writing Courses and Projects
Adrienne Herron
Article written for The Low Down
published in Artists of the Gatineau Hills, 2007
Adrienne Herron, Coming Full Circle
Adrienne Herron lives in the quiet where she photographs the ever-changing mysteries of Nature. Surrounded by the serene shade gardens she has created, she finds the solitude to see into the life of things – the way a leaf turns, the blur of detail when the camera moves to encompass a stand of trees or to evoke an impressionist painting of the subtlest colours.
She frequently visits a neighbouring orchard that has become for her a sanctuary of light and shadow. Under the pressure of expanding development, it may soon be lost but not before she has honoured its delicate presence. "I want to capture not only the beauty, power and grace of trees, but their intense and imminent vulnerability."
Adrienne received her first camera, a baby Brownie, for Christmas the year she turned 8. The family had just moved from Toronto to Montreal after her father, an American photographer, returned to the States. She would not see him again for thirty years. And yet his influence would help to shape her own destiny as an artist – a passion for photography that has never left her.
"It is my lifeline to who I really am. You can lose your connection to life without creativity. It feeds your soul. I love being in the woods – they are magical. Photography allows me to look more closely, to realize the symbiotic relationship we have with trees, with all of Nature. It's a metaphor for how we stay alive."
Throughout a long career in marketing, training and sales for QL Systems – an information retrieval service for lawyers called QUICKLAW – Adrienne pursued her photography studies at Algonquin, Carleton, and at workshops across the States and Canada, culminating in a BFA from Ottawa University in 2001. She has exhibited widely, both in solo and group exhibitions throughout the region. Known for her inspired photography and art programs in Giverny, France (1996-1999), Adrienne taught photography for over ten years and created the "Image Bank" for the Gatineau Valley Historical Society.
There is a circle here in the path she has taken. Reconnecting with her father, as an adult, brought the riches of his experience into her life. She would send him photographs and he would critique them, sharing his secret formulas, challenging her to push further. Following in his footsteps anchored her passion, brought her heritage home.
And so too the work itself has carried her full circle. Just as the invention of photography usurped the province of painting, forcing painters to differentiate, away from Realism into Impressionism, now Adrienne is experimenting with the reverse crossover. "I want to do what the camera shouldn't be able to do – to move away from harsh reality, from detail, into a more minimalist, painterly effect."
Camera movement fascinates her – capturing the spirit of place. "I follow. I don't direct. The not knowing is the adventure. It's like a spiritual quest. My photographs are a series of epiphanies – I don't want to miss anything."
Transient Forest Series, 9482e
cathjoyce66@gmail.com
© 2022 Catherine Joyce All Rights Reserved.
Theme by Theme Trust


Grid operator National Grid Corp. of the Philippines said it is constructing the Pagbilao 500-kilovolt substation project to support large capacity generation and address the rising demand for power.
The Pagbilao substation project is one of NGCP's efforts to address transmission issues in Quezon province and accommodate incoming power generation, which include the 420-megawatt Pagbilao coal-fired power plant expansion, 500-MW San Buenaventura coal-fired power plant and 600-MW Energy World Corp.'s combined-cycle power plant.
Quezon province hosts two of the major power plants in the Luzon grid including the 735-MW Pagbilao coal-fired power plant and the 460-MW Quezon Power coal-fired power plant.
"With over 1500 MW of power coming into the grid once these plants are online, we need a new gateway of power in the Quezon province which can fully accommodate all these. The Pagbilao 500kV substation will help ease voltage and load issues of nearby substations like Tayabas, and further enhance transmission of power not only in Quezon province but in the entire Luzon grid as well", NGCP said.


Trash must be removed to containers placed under house every night, do not store it on the floor please.
Interaction with guestsCount on me for any questions or need, whether it's in my hand, I will do everything possible to make your stay easier and more enjoyable. We do not ask for anything other than common sense and act in the same way as if it were your own home. The apartment is accessed via two portals, the left takes you to the elevator and the right to the stairs. Garbage containers must get that place at night on the street, from 20:00.
The apartment is located a few meters from food shops and supermarkets. It is a quiet and convenient to move to anywhere in the city in just 20 minutes neighborhood. The apartment is very close to Ciudad Universitaria.
A few steps you will find the number 44 bus stop that will take you to the city center. The house is situated in between stops Cuatro Caminos subway and Guzmán El Bueno.


text:
Colin Powell: 'We've come to live in a society based on insults, on lies'
By Brett Samuels - 10/31/18 03:07 PM EDT
Former Secretary of State Colin Powell said on Tuesday that the U.S. has become a society based on "insults" and "lies," cautioning that the deterioration of public discourse is hurting America's reputation abroad.
"We have come to live in a society based on insults, on lies and on things that just aren't true. It creates an environment where deranged people feel empowered," Powell, who served under former President George W. Bush (R), said during an event at Creighton University in Omaha, Neb., according to CNN.
"We've seen incidents before but now, we've come to live in a society based on insults and attacking almost every facet of American life," he added.
Powell also called on "all public officials" to work with members of the other party and to cool political hostilities following a series of bomb threats against prominent Democrats and CNN and a massacre at a synagogue in Pittsburgh.
The 81-year-old former Cabinet official has been critical of President Trump Donald TrumpClinton, Bush, Obama reflect on peaceful transition of power on Biden's Inauguration Day Arizona Republican's brothers say he is 'at least partially to blame' for Capitol violence Biden reverses Trump's freeze on .4 billion in funds MORE in the past, and has questioned whether he can be a moral leader for the country.
In Nebraska, Powell was specifically critical of the president's rhetoric toward immigrants, and particularly a group of Central American migrants making its way toward the southern U.S. border. Trump has painted the group as an imminent threat to national security, spreading unfounded claims that "unknown Middle Easterners" and "thugs" are traveling with the group.
"This is a disgrace," Powell said. "I don't see any terrorists. I don't see any bombs going off. I'm not saying we let everybody in, you don't just open the door. But we should avoid language like this and see how we can solve this problem."
Tags Donald Trump political rhetoric lies


text:
\section{Introduction}

Understanding the production of nuclides heavier than iron is a crucial part of our global quest to understand the origin of the elements. The slow neutron capture process ($s$-process) is a key contributor to heavy-element synthesis, producing around $50\%$ of the nuclides heavier than iron in our solar system. The $s$-process occurs in relatively moderate stellar environments---the He-shell burning phase of intermediate-mass asymptotic giant branch (AGB) stars and the He-core and C-shell burning phases of massive ($M > 8M_{\odot}$) stars---and involves a series of neutron capture reactions on stable or near-stable nuclei \cite{Kappeler2011}. Neutron capture rates on stable isotopes are typically known to an accuracy of $20\%$ or better, and hence the $s$-process offers a prime opportunity to compare predicted nucleosynthesis yields with astronomical observations and meteorite and stardust analyses \cite{Kappeler2011,Karakas2012,Clayton2004,Lugaro2005}. However, there are still a number of key outstanding nuclear physics uncertainties surrounding the $s$-process---in particular, neutron capture rates on branching-point nuclides, as well as uncertainties related to the overall neutron flux. Neutron generation during the weak $s$-process, which occurs during the He-core and C-shell burning phases in massive stars, is dominated by the $^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ reaction. The rate of this reaction, as well as the competing $^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ reaction, is not well constrained in the relevant temperature range for the weak $s$-process, significantly impacting predicted nucleosynthesis yields.
For example, recent calculations indicate that varying the $^{22}$Ne($\alpha,n$)$^{25}$Mg rate within existing uncertainties leads to a factor of ten or greater changes in predicted weak $s$-process yields throughout the $A \sim 60$--$90$ mass region \cite{Longland2012,Talwar2016}.

The astrophysical impact of the $^{22}$Ne($\alpha,\linebreak[1] n$)$^{25}$Mg and $^{22}$Ne($\alpha,\linebreak[1]  \gamma$)$^{25}$Mg reactions is not limited to the $s$-process. They also affect synthesis of the long-lived $\gamma$-ray emitters such as $^{60}$Fe, created through ${}^{59}$Fe$(n,\gamma){}^{60}$Fe with $^{22}$Ne($\alpha,n$)$^{25}$Mg serving as a neutron source in the high-temperature ($T \sim 1$~GK) C-shell burning phase of massive stars. The $\gamma$-ray emission from $^{60}$Fe has been observed together with $^{26}$Al, another long-lived $\gamma$-ray emitter, by low-energy $\gamma$-ray telescopes such as INTEGRAL \cite{Wang2007}. Their abundance ratio is considered a key constraint on massive-star nucleosynthesis models and galactic chemical evolution \cite{Diel2010}. Furthermore, estimated chemical abundances based on established $s$-process models provide estimates of the less well-known solar $r$-process abundances. Hence a better understanding of $s$-process nucleosynthesis is helpful in working towards a complete understanding of the $r$-process in the era of multi-messenger astronomy.

At stellar temperatures, both $^{22}\mathrm{Ne}(\alpha,\linebreak[1] n){}^{25}\mathrm{Mg}$ and $^{22}\mathrm{Ne}(\alpha,\linebreak[1] \gamma){}^{26}\mathrm{Mg}$ proceed through resonant capture to natural-parity states in the compound nucleus, $^{26}\mathrm{Mg}$. For a given resonance, the key properties determining its contribution to the stellar rate are the $\alpha + {}^{22}\mathrm{Ne}$ resonance energy and the resonance strengths, $\omega\gamma_{(\alpha,n)}$ and $\omega\gamma_{(\alpha,\gamma)}$.\footnote{The resonance strengths are given by $\omega\gamma_{(\alpha,n)} \simeq (2J+1)\Gamma_{\alpha}/(1+\Gamma_{\gamma}/\Gamma_n$) and $\omega\gamma_{(\alpha,\gamma)} \simeq (2J+1)\Gamma_{\alpha}/(1+\Gamma_{n}/\Gamma_\gamma$), taking the approximation $\Gamma_\alpha \ll \Gamma$. Here, $J$ is the resonance spin, and $\Gamma_\alpha$ ($\Gamma_n,$ $\Gamma_{\gamma}$, $\Gamma$) is the $\alpha$ (neutron, $\gamma$-ray, total) partial width.}
Above $0.3$~GK, both the $(\alpha,n)$ and $(\alpha,\gamma)$ reactions are dominated by a resonance at $E_{cm} = 0.703$~MeV ($E_x=11.32$~MeV). This resonance has been observed in both direct $(\alpha,n)$ \cite{Harms1991, Drotleff1993, Giesen1993, Jaeger2001} and $(\alpha,\gamma)$ experiments \cite{Wolke1989,Hunt2019}, although there is disagreement about whether or not these are the same state \cite{Koehler2002, Longland2012, Adsley2017}.
The $(\alpha,\gamma)$ strength is well established, with both published measurements \cite{Wolke1989, Hunt2019} in good agreement, as well as with the unpublished result of Jaeger \cite{JaegerPhD}. In contrast, the resonance strengths extracted from the direct $(\alpha,n)$ measurements are in poor agreement, suggesting the presence of an unknown systematic bias in the data \cite{Longland2012}. As a result, $\omega\gamma_{(\alpha,n)}$ for the $E_x=11.32$~MeV  resonance remains a key outstanding uncertainty on the total $^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ rate at stellar temperatures. Additionally, the spin-parity of this resonance is not firmly established, and most recently it was suggested that $J^\pi = (0^+,$ $1^-$, $2^+$, $3^-$) are all allowable \cite{Hunt2019}. Although $J^\pi$ does not affect the direct-measurement strengths, it is a crucial parameter for extracting $\omega\gamma_{(\alpha,n)}$ from indirect $\alpha$ transfer studies \cite{Giesen1993, Talwar2016}. Additionally, it affects the scaling factors used to extract $\Gamma_\alpha$ for lower-lying resonances from $\alpha$ transfer \cite{Talwar2016}.

\revised{
At lower temperatures, both reactions \emph{may} be dominated by one or more resonances between the neutron threshold and $E_{cm} \sim 0.635$~MeV ($E_x \sim 11.25$~MeV). The presence of an important resonance in this region has long been controversial. \etal{Giesen}, in their  (\nuc{6}{Li},~$d$) experiment, observed no strong transitions in this energy region \cite{Giesen1993}. They set an upper limit of $S_\alpha < 0.02$ on a candidate $1^-$ resonance at $E_x=11.15$~MeV originally identified in  photoneutron \cite{Berman1969} and neutron capture \cite{Weigmann1976} studies. Assuming $J=1$ and contemporary values for $\Gamma_n$ and $\Gamma_\gamma$, this resulted in respective limits on the $(\alpha,n)$ and $(\alpha,\gamma)$ strengths of $\omega\gamma_{(\alpha,\gamma)} < 0.097~\mu$eV and $\omega\gamma_{(\alpha,n)} < 0.74~\mu$eV.
 \etal{Jaeger} also searched for this state in their direct $(\alpha,n)$ measurement, setting an upper limit on the resonance strength of $\omega\gamma_{\alpha,n} < 60~$neV. This state was later shown to be a $1^+$ (non-natural parity) and thus completely inconsequential to either $\alpha$ capture reaction \cite{Longland2009}.

In the later (\nuc{6}{Li},~$d$) measurement at higher beam energy, Talwar \textit{et al}.\ observed a strong transition at $E_x = 11.167(8)$~MeV \cite{Talwar2016}. They also observed a transition at a similar energy in their concurrent $^{26}\mathrm{Mg}(\alpha,\alpha^\prime){}^{26}\mathrm{Mg}$ experiment. They assigned a spin-parity of  $J^\pi = (1^-, 2^+)$ and extracted a spectroscopic factor of  $S_\alpha=0.36$, corresponding to $\Gamma_\alpha = 0.18(2)~\mu$eV when taking their preferred spin-parity assignments. In order to maintain consistency with the $\omega\gamma_{(\alpha,n)}$ upper limit of \etal{Jaeger}, they attributed the additional strength to the $(\alpha,\gamma)$ channel, establishing $\omega\gamma_{(\alpha,\gamma)} = 0.54(7)~\mu$eV. Based on these results, the authors established that this state dominates the ${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}${} rate between ${\sim}0.2$--$0.4~$GK and that it could potentially dominate the ${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}${} rate below $0.2$~GK.
More recently, neutron capture studies by Massimi \emph{et al}.\ have identified four natural-parity resonances in the ${}^{26}\mathrm{Mg}$ excitation energy range from $11.1$--$11.3$~MeV \cite{Massimi2012, Massimi2017}. Three of these resonances were found to stongly neutron decay, while the fourth, $E_x = 11.171$~MeV, was identified as a $2^+$ state with a significant $\gamma$-ray decay branch ($\Gamma_{n}/\Gamma_\gamma = 0.2$--$6$). This makes it a candidate for the strong $(\alpha,\gamma)$ resonance claimed in Ref.~\cite{Talwar2016}.
}

Despite extensive investigaton \cite{Wolke1989,Harms1991, Drotleff1993, Giesen1993, Jaeger2001,Koehler2002, Ugalde2007, Schwengner2009, Longland2009, deBoer2010, Massimi2012, Ota2012, deBoer2014, Ota2014, Talwar2016, Massimi2017, Adsley2017, Adsley2018, Hunt2019, Longland2012, JaegerPhD, Berman1969, Weigmann1976}, key properties of both the $E_x = \linebreak[1] 11.32$ MeV resonance and lower-lying neutron-unbound resonances remain uncertain. In particular, the $(\alpha,n)$ strength of the  $E_x = 11.32$~MeV resonance is not well established, nor is its spin-parity.
The situation for lower-lying resonances is even less clear, with substantial disagreement between existing $({}^6\mathrm{Li},d)$ experiments about the presence of a strong $\alpha$-cluster state around $E_x = 11.17$~MeV. Additionally, the $\alpha$ partial widths for the natural-parity resonances identified by Massimi \emph{et al}.\ remain poorly constrained, with the lowest-lying resonance, $E_x = 11.112$~MeV, having the potential to completely dominate the $(\alpha,n)$ rate below ${\sim}0.3$~GK.

Here we report a new, kinematically-complete measurement of the ${}^{22}\mathrm{Ne}({}^6\mathrm{Li}, d){}^{26}\mathrm{Mg}$ reaction in inverse kinematics, with direct sensitivity to the decay modes of observed states. The sensitivity to decay modes is a key advantage of the present study, allowing us to simultaneously address a number of questions surrounding both the $^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ and $^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ reactions. In particular, we report a new value of $\Gamma_n / \Gamma_{\gamma}$ for the $E_x = 11.32$~MeV resonance that is a factor ${\sim}3$ below the value extracted from direct measurements.
Furthermore, in the region between the neutron threshold and $E_x = 11.25$~MeV, the sensitivity to decay modes allows us to set stringent limits on the ${}^{22}\mathrm{Ne}({}^6\mathrm{Li}, dn){}^{25}\mathrm{Mg}$ cross section, which translates into an upper limit on $\Gamma_{\alpha} \Gamma_{n}/\Gamma$. Taken in conjunction with the resonance parameters ($J$, $\Gamma_{n}$, $\Gamma_{\gamma}$) established by Massimi \emph{et al}., this results in new upper limits on both the $(\alpha,n)$ and $(\alpha,\gamma)$ strengths for the four natural-parity states in this region identified in Refs.~\cite{Massimi2012, Massimi2017}.

\section{Methodology and Results}
The experiment was performed at the Texas A\&M University Cycloton Institute, using the K150 cyclotron to deliver a beam of 154~MeV $^{22}$Ne$^{(7+)}$ ions, impinging on a 30~$\mu$g/cm$^2$ $^{6}$LiF target (95\% \nuc{6}{Li} purity), with a 10 $\mu$g/cm$^2$ carbon backing. Our detector system consisted of the TIARA Si array \cite{Labiche2010}, four closely-packed HPGe clovers \cite{Lesher2010}, and the MDM spectrometer \cite{Pringle1986}. The acceptance of the MDM was $\pm 2^\circ$ in both the dispersive and non-dispersive planes, defined by rectangular slits at its entrance.
Target-like deuterons were detected in the backward hemisphere ($\theta_{lab}$ = 148$^\circ$--168$^\circ$) by a double-sided annular Si detector and were used to reconstruct the excitation energy of $^{26}$Mg states from the missing mass. Elastically scattered target nuclei were detected in a series of resistive strip detectors in a barrel configuration ($\theta_{lab}$ = 45$^\circ$--145$^\circ$).
Beam-like \nuc{26}{Mg} (\nuc{25}{Mg}) recoils resulting from $\gamma$-ray (neutron) decay of $^{26}$Mg excited states were unambiguously identified in the MDM focal plane using a combination of energy loss, total energy, and dispersive position signals from the upgraded Oxford detector \cite{Spiridon2016,Spiridon2019}, as demonstrated in Figure~\ref{fig:PID}.  The identification of ${}^{25,26}$Mg recoils was confirmed by the coincident $\gamma$-ray transitions measured in the HPGe detectors. The clear identification of both recoil species with good efficiency allowed reliable extraction of $\Gamma_n/\Gamma_\gamma$ for $^{26}$Mg states populated in the $({}^6\mathrm{Li},d)$ reaction, from the efficiency-corrected ratio of ${}^{25}\mathrm{Mg}/{}^{26}\mathrm{Mg}$ recoils in coincidence with the state of interest.

\revised{
These recoil detection efficiencies are the product of the spectrometer acceptance, the Mg charge state fraction, and the intrinsic detection efficiency of the focal plane detectors. The charge state fraction is identical for \nuc{25,26}{Mg} and hence cancels in the final ratio used to calculate $\Gamma_n/\Gamma_\gamma$. The intrinsic detection efficiency was estimated to be $80.0(20)\%$. This was calculated from the ratio of ${}^{23}\mathrm{Ne} + d$ coincidences to deuteron singles observed for strongly-populated singlet states in a separate ${}^{22}\mathrm{Ne}(d,p){}^{23}\mathrm{Ne}$ run using the same setup. Due to the small cone angle of the $(d,p)$ reaction,  the \nuc{23}{Ne} acceptance here was $100\%$. The intrinsic efficiency again cancels in the $\Gamma_n/\Gamma_\gamma$ calculation; however, the $\pm 2.0\%$ uncertainty, which comes from the observed variation in $(d,p)$ coincidence/singles ratios over different proton angular bins, was propagated into the final \nuc{25}{Mg}/\nuc{26}{Mg} efficiency ratio.
Acceptances for \nuc{25}{Mg} and \nuc{26}{Mg} recoils were determined from Monte Carlo simulations  performed using the NPTOOL  interface to the GEANT4 framework \cite{Matta2016}. The simulations impinged a \nuc{22}{Ne} beam with realistic energy spread and emittance onto the target and generated deuterons and \nuc{26}{Mg} recoils from standard four-momentum conservation in the $({}^{6}\mathrm{Li},d)$ reaction. For the ${}^{25}\mathrm{Mg} + d$ case, the \nuc{26}{Mg} recoils were subsequently broken up into ${}^{25}\mathrm{Mg}^{\mathrm{(g.s.)}}  + n$ assuming an isotropic distribution (only the \nuc{25}{Mg} ground state is energetically accessible for $E_x \leq 11.68$~MeV). The resulting \nuc{25,26}{Mg} recoils, in coincidence with deuteron angles detected in the experiment, were then propagated to the focal plane of the MDM. A first set of acceptance cuts was placed at the location of the $\pm 2^\circ$ slits at the spectrometer entrance. Recoils passing these cuts were then propagated to the end of the spectrometer using a well-characterized RAYTRACE transport code \cite{Pringle1986}. The final set of acceptance cuts was placed at the entrance window to the Oxford detector, which was $\pm 15$~cm and $\pm 3$~cm in the dispersive and non-dispersive planes, respectively. To account for spin dependence, separate simulation runs were performed for $L=0,1,2$ transitions and the weighted average was taken as the final acceptance.
The acceptances of  \nuc{25}{Mg} and \nuc{26}{Mg} recoils were determined to be $77.8(11)\%$ and $90.8(5)\%$, respectively, resulting in a \nuc{25}{Mg}/\nuc{25}{Mg} efficiency ratio of $0.858(33)$.
}

\begin{figure}
	\centering
 \includegraphics[width=8cm]{Fig_PID.pdf}
 \caption{a) Energy loss vs.\ total energy measured in the Oxford detector, showing separation of Mg isotopes from other species. b) Energy loss vs.\ focal plane position, gated on the Mg band in panel (a) and showing clear separation of \nuc{25}{Mg} and \nuc{26}{Mg}.\label{fig:PID}}
 \end{figure}

\begin{table}
\centering
	\footnotesize
\begin{threeparttable}
	\caption{\label{tab:Tab1}Optical parameters used in FRESCO for the DWBA analysis of $^{22}\mathrm{Ne}({}^6\mathrm{Li}, d){}^{26}\mathrm{Mg}$. All radii except those for the $\alpha + d$ channel are given such that $R_x = r_x  A_T^{1/3}$. For the $\alpha + d$ channel, $R_x=r_x$. }
\begin{tabular}{cccccccc
\hline
			\multirow{2}{*}{Channel} &
		           $r_c$ & $V_r$ & $r_r$ & $a_r$ & $W_s$ & $r_I$ & $a_I$ \\%& $W_D$ & $r_D$ & $a_D$ & $V_{so}$ & $r_{so}$ & $a_{so}$  \\
		     	  & (fm)  & (MeV) & (fm)  & (fm)  & (MeV) & (fm)  & (fm)  \\%& (MeV) & (fm)  & (fm)  & (MeV)    & (fm)     & (fm)      \\
\hline
       $^{22}$Ne+$^6$Li & 1.30  & 117.04& 1.80  & 0.40  & 48.6  & 1.99  & 0.62  \\%&       &       &          &          &     \\
       $^{26}$Mg+$d${\tnote{a}} & 1.30  & 79.07 & 1.17  & 0.79  & 2.99  & 1.325 & 0.737 \\%& 10.51 & 1.325 & 0.737 & 5.88 & 1.07 & 0.66\\
$\alpha$+$d$             & 1.90  & {\tnote{b}}  & 1.90  & 0.65  &       &       &       \\%&       &       &       &      &      &     \\
Final State              & 1.40  & {\tnote{c}}  & 1.40  & 0.70  &       &       &       \\%&       &       &       &      &      &     \\
\hline
\end{tabular}
\begin{tablenotes}
	\item[a]{In addition, the following parameters were used for ${}^{26}\mathrm{Mg} + d$ channel: $W_D=10.51$~MeV,
$V_{so}=5.88$~MeV, $r_{so}=1.07$~fm, and $a_{so}=0.66$~fm.}
	\item[b]{Adjusted to give the correct $^6$Li binding energy.}
	\item[c]{Adjusted to give the correct final state binding energy.}
\end{tablenotes}
\end{threeparttable}
\end{table}

Figure~\ref{fig:Fig2}(a) shows the angle-integrated ($\theta_{CM} = 6^{\circ}$--14$^{\circ}$) $^{26}$Mg excitation energy spectrum measured by the annular Si detector. A number of strongly populated states (both bound and unbound) are evident, and the overall features of the spectrum agree well with past measurements \cite{Anantaraman1977, Giesen1993, Talwar2016}. Figure~\ref{fig:Fig2}(c) shows the angular differential cross section (arbitrarily normalized) for the $E_x =11.32$~MeV resonance. Distorted Wave Born Approximation (DWBA) calculations for various $J^\pi$ values are also shown.   The calculations were performed with the FRESCO code \cite{Thompson1988, Thompson2009}, using the optical potential parameters presented in Table~\ref{tab:Tab1}. The optical potential parameters were arrived at by using the SFRESCO minimization routine to best fit the digitized $^{22}\mathrm{Ne}({}^6\mathrm{Li}, d){}^{26}\mathrm{Mg}$ data from Ref.~\cite{Anantaraman1977}, for strongly-populated states with known spin. SFRESCO was used to adjust both the $^6\mathrm{Li} + {}^{22}$Ne optical potentials (starting from those published in Ref.~\cite{Cook1982}) and the $\alpha + {}^{22}$Ne overlap potentials. The  potentials for $d + {}^{26}$Mg and $\alpha + d$ were taken from Refs.~\cite{Daehnick1980, Nishioka1984} and left fixed. For the internal-state ($\alpha$--$d$ system) in the $^{6}$Li nucleus, a relative $2S$ state was assumed \cite{Anantaraman1977}. For the final state in the $^{26}$Mg nucleus, the number of radial nodes was fixed by the harmonic oscillator energy conservation relation, assuming an $(sd)^4$ configuration for the positive parity states and an $(sd)^3(fp)$ configuration for the negative parity states.
For resonance states,  $J^\pi$ radial wave functions, computed using the final-state $\alpha + {}^{22}\mathrm{Ne}$ potential, were used

\begin{figure*}
	\centering
 \hspace*{-1.25in}
 \includegraphics[width=18cm]{Ex_angdist-fits-3panel.pdf}
 \caption{a) $^{26}$Mg excitation energy spectrum measured from the $^6\mathrm{Li}({}^{22}\mathrm{Ne},d){}^{26}$Mg reaction at $\theta_{CM} = 6^{\circ}$--14$^{\circ}$. The red shaded area represents deuterons in coincidence with $^{26}$Mg, while the blue curve is the sum of $^{25}$Mg and $^{26}$Mg coincidences. b) Results of the multi-Gaussian fit explained in the text. Separate fits are shown for $({}^{6}\mathrm{Li}, dn)$ and $({}^{6}\mathrm{Li}, d\gamma)$ as indicated. The black dotted curves represent the individual Gaussian peaks, and the red solid curve is their sum. Nominal energies of each peak included in the fit are enumerated in the figure. c) Angular differential cross section (arbitratily normalized) to the $E_x = 11.32$~MeV state, along with the DWBA calculations explained in the text. The inset shows the individual $^{22}\mathrm{Ne}({}^{6}\mathrm{Li},dn){}^{25}\mathrm{Mg}$ and $^{22}\mathrm{Ne}({}^{6}\mathrm{Li},d\gamma){}^{26}\mathrm{Mg}$ cross sections, as indicated. \label{fig:Fig2}}
 \end{figure*}

\subsection{11.32 MeV Resonance}\label{sec:1132}
A peak at $E_x$ = 11.32 MeV is clearly present in the summed ${}^{25}\mathrm{Mg} + {}^{26}\mathrm{Mg}$ excitation energy spectrum, with approximately equal numbers of \nuc{25,26}{Mg} coincidences. As shown in Figure~\ref{fig:Fig2}(c), the shape of our summed ${}^{25}\mathrm{Mg} + {}^{26}\mathrm{Mg}$ angular distribution is consistent with the $J^\pi = (0^{+},~1^-)$ calculations and not consistent with  $J^\pi = (2^{+},~3^-)$. The angular distributions for the neutron and $\gamma$-ray decay channels are statistically identical in shape, as demonstrated in the inset of Figure~\ref{fig:Fig2}(c). This strongly suggests that the resonances observed in independent $(\alpha,n)$ and $(\alpha,\gamma)$ direct measurements are indeed the same state and not a doublet as suggested in Refs.~\cite{Longland2012, Adsley2017}. Owing to the lack of reliable beam-on-target normalization, we were unable to extract absolute $\alpha$ spectroscopic factors for the $E_x=11.32$~MeV state. Instead, we determine relative spectroscopic factors by normalizing to the published direct-measurement $(\alpha,\gamma)$ strength, combined with the presently-reported $\Gamma_{n}/\Gamma_{\gamma}$. For the direct-measurement strengths, we take the weighted average of Refs.~\cite{Wolke1989,Hunt2019}, $37(4)~\mu$eV. From the spectroscopic factors obtained using this procedure, we calculate spin-dependent values of $\Gamma_{\alpha}$ using the prescription of Ref.~\cite{Thompson2009}. The results are presented in Table~\ref{tab:Table2}, assuming both $0^+$ and $1^-$ assignments.

\revised{
To extract the $\Gamma_n / \Gamma_\gamma$ for the $E_x = 11.32$~MeV resonance, we performed a multiple-Gaussian fit to the region around  $E_x = 11.32$~MeV in the individual ${}^{25}$Mg- and ${}^{26}$Mg-gated spectra. The amplitude of each Gaussian was allowed to vary freely, and the central energies and widths were restricted based on existing experimental information and knowledge of the experimental setup, as described below.
In the fit, we included all states previously observed in $({}^{6}\mathrm{Li},d)$ by either of Refs.~\cite{Giesen1993, Talwar2016}. The nominal central energies of each of these peaks are enumerated in Figure~\ref{fig:Fig2}(b). To account for uncertainties in the peak energy,  the centroid of each Gaussian was allowed to vary by $\pm 10$~keV from the nominal---with the exception of the peak at ${\sim} 11.17$~MeV. Because multiple natural-parity states have been identified in the region around 11.17~MeV \cite{Massimi2017}, and furthermore because of the controversy between Ref.~\cite{Giesen1993} and Ref.~\cite{Talwar2016} concerning the presence of a low-spin, strong $\alpha$ cluster state in this region, we allowed for a greater uncertainty in the central energy of the peak in this region. Specifically, we allowed the central energy of this peak to vary freely between 11.1 and 11.25~MeV. Because of the astrophysical interest of this state, we also extracted an upper limit on its spectroscopic factor, as explained in Section~\ref{sec:11171}.
The width of each peak was allowed to vary by $\pm 11.8$~keV FWHM ($\sigma= \pm 5$ keV) from the nominal resolution of $230$~keV FWHM. The resolution was determined from a GEANT4 Monte Carlo simulation that included the the effects of target thickness, beam emittance and energy spread, and Si energy and angular resolution. The accuracy of the simulation was verified by comparing the results to experimental data for strongly populated states.
}

The results of the fitting procedure are shown in Figure~\ref{fig:Fig2}(b), overlayed with the present experimental data. The total number of counts in the \nuc{25}Mg- and \nuc{26}{Mg}-gated, $1.32$~MeV peaks were extracted from the areas under the respective \nuc{25}Mg- and \nuc{26}{Mg}-gated Gaussians centered at 11.32 MeV. Their efficiency-corrected ratio resulted in a branching ratio $\Gamma_n/\Gamma_\gamma = 1.14(26)$.
Normalizing to $\omega\gamma_{(\alpha,\gamma)} = 37(4)~\mu$eV,  we obtain a new $^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ strength of $\omega\gamma_{(\alpha,n)} = 42(11)~\mu$eV. While this strength agrees within $2\sigma$ with the direct measurement of Harms \emph{et al}., $83(24)~\mu$eV \cite{Harms1991}, it disagrees by more than $2\sigma$ with all other direct measurements. In particular it disagrees by $5.0\sigma$ with the most recently published result of Jaeger \emph{et al.}, $118(11)~\mu$eV \cite{Jaeger2001}, and by $3.1\sigma$ with the inflated weighted average of $140(30)~\mu$eV calculated by  Longland \emph{et al}.\ \cite{Longland2012}.

The  implications of the presently-established $(\alpha,n)$ resonance strength are fully realized when it is combined with the $\Gamma_\alpha$ concurrently reported in a sub-Coulomb ${}^{6}\mathrm{Li}({}^{22}\mathrm{Ne},\linebreak[1] d){}^{26}\mathrm{Mg}$ and ${}^{7}\mathrm{Li}({}^{22}\mathrm{Ne},\linebreak[1] t){}^{26}\mathrm{Mg}$ study by Jayatissa \emph{et al}.\ \cite{Jayatissa2019}. As explained in that work, the present $\Gamma_n/\Gamma_\gamma$ can be combined with the direct-measurement $(\alpha,\gamma)$ strength of $37(4)~\mu$eV to calculate $\alpha$ partial widths of $79(13)$, $26(4)$, and $16(3)~\mu$eV for respective $J=0,$ $1$, and $2$ spin assignments. The respective levels of agreement with the sub-Coulomb results are $1.1\sigma$, $2.8\sigma$, and $5.0\sigma$. This strongly suggests a $J^\pi=0^+$ assignment for this state, although the $1^-$ assignment cannot be conclusively ruled out. These assignments agree with the present angular distributions, shown in Figure~\ref{fig:Fig2}, which are consistent with $J=(0,1)$.

A similar argument to the one above suggests that the $\omega \gamma_{(\alpha,n)}^{(11.32)}$ reported in direct measurements are seriously overestimated.
\revised{
If we instead take $(2J+1)\Gamma_\alpha = \omega\gamma_{(\alpha,n)}+\omega\gamma_{(\alpha,\gamma)}$, with $\omega\gamma_{(\alpha,n)}$ and $\omega\gamma_{(\alpha,\gamma)}$ both from direct measurements, even the $J^\pi = 0^+$ results disagree substantially with  Ref.~\cite{Jayatissa2019}.
}
For example, using $\omega\gamma_{(\alpha,n)}= 118(11)~\mu$eV \cite{Jaeger2001} results in $\Gamma_\alpha^{(J=0)} = 155(12)~\mu$eV, a $5.9\sigma$ discrepancy. Similarly, using the inflated weighted average presented by Longland \emph{et al}., $\omega\gamma_{(\alpha,n)}= 140(30)~\mu$eV, results in $\Gamma_\alpha^{(J=0)} = 177(30)~\mu$eV, a $3.6\sigma$ discrepancy.

\begin{table*}
	\centering
	\footnotesize
	\begin{threeparttable}
		\caption{\label{tab:Table2}Resonance parameters determined for the $^{26}$Mg $11.32$~MeV state and natural parity states between the neutron threshold and 11.25~MeV identified in Refs.~\cite{Massimi2012, Massimi2017}. All upper limits are quoted at $90\%$ CL, and uncertainties in parentheses are quoted at $1\sigma$ ($68\%$ CL).}
\begin{tabular}{ccccccccc}
\hline
	$E_x$ & $E_{cm}$ & \multirow{2}[0]{*}{$J^\pi$} & \multirow{2}[0]{*}{${\Gamma_n}/{\Gamma_\gamma}$} & \multirow{2}[0]{*}{$S_\alpha$} & $\Gamma_\alpha$ & $\omega\gamma_{tot}$ & $\omega\gamma_{(\alpha,\gamma)}$ & $\omega\gamma_{(\alpha,n)}$ \\
	(MeV) & (MeV) &       &       &       & (eV)  & (eV)  & (eV)  & (eV) \\
\hline
	11.112 & 0.497 & $2^+$\tnote{a} & 1530\tnote{a} & $<0.025$\tnote{b} & $<2.2\ee{-10}$\tnote{b} & $<1.1\ee{-9}$ & $<7.1\ee{-13}$ & $<1.1\ee{-9}$ \\
	&      &       &                                & $<0.043$\tnote{c} & $<4.3\ee{-10}$\tnote{c} & $<2.1\ee{-9}$ & $<1.4\ee{-12}$ & $<2.1\ee{-9}$ \\
	11.163 & 0.548 & $2^+$\tnote{a} & 1900\tnote{a} & $<0.025$\tnote{b} & $<2.7\ee{-9}$\tnote{b}  & $<1.4\ee{-8}$ & $<7.2\ee{-12}$ & $<1.4\ee{-8}$ \\
	&      &       &                                & $<0.043$\tnote{c} & $<5.2\ee{-9}$\tnote{c}  & $<2.6\ee{-8}$ & $<1.4\ee{-11}$ & $<2.6\ee{-8}$ \\
	11.169 & 0.554 & $3^-$\tnote{a} & 588\tnote{a}  & $<0.024$\tnote{b} & $<4.4\ee{-10}$\tnote{b} & $<3.1\ee{-9}$ & $<5.2\ee{-12}$ & $<3.1\ee{-9}$ \\
	&      &       &                                & $<0.041$\tnote{c} & $<1.1\ee{-11}$\tnote{c} & $<5.9\ee{-9}$ & $<1.0\ee{-11}$ & $<5.9\ee{-9}$ \\
	11.171 & 0.556 & $2^+$\tnote{a} & 0.2\tnote{a}  & $<0.15$\tnote{b}  & $<1.9\ee{-8}$\tnote{b}  & $<9.6\ee{-8}$ & $<8.0\ee{-8}$  & $<1.6\ee{-8}$ \\
	&      &       &                                & $<0.26$\tnote{c}  & $<3.7\ee{-8}$\tnote{c}  & $<1.9\ee{-7}$ & $<1.6\ee{-7}$  & $<3.1\ee{-8}$ \\
	11.318 & 0.703 & $0^+$ & $1.14(26)$ & $0.31(5)$\tnote{d} & $7.9(13)\ee{-5}$\tnote{d} & $7.9(13)\ee{-5}$ & $3.7(4)\ee{-5}$\tnote{e} & $4.2(11)\ee{-5}$\tnote{d} \\
	             &             & $1^-$  & $1.14(26)$ & $0.18(3)$\tnote{d} & $2.6(4)\ee{-5}$\tnote{d}  & $7.9(13)\ee{-5}$ & $3.7(4)\ee{-5}$\tnote{e} & $4.2(11)\ee{-5}$\tnote{d} \\
\hline
\end{tabular}%
		\begin{tablenotes}
			\item[a]{Adopted from Refs.~\cite{Massimi2012, Massimi2017}.}
			\item[b]{Normalized to $S_\alpha^{(E_x=11.32)}$, assuming $J^\pi=0^+$. }
			\item[c]{Normalized to $S_\alpha^{(E_x=11.32)}$, assuming $J^\pi=1^-$. }
			\item[d]{Normalized to $\omega\gamma_{(\alpha, \gamma)} = 37(4)~\mu$eV and $\Gamma_{n}/\Gamma_{\gamma}=1.14(26)$.}
			\item[e]{Weighted average of Refs.~\cite{Hunt2019, Wolke1989}.}
		\end{tablenotes}
	\end{threeparttable}
\end{table*}

\subsection{Resonances Below 11.32 MeV}
\label{sec:11171}

\revised{
Between the neutron threshold and $E_x = 11.32$~MeV, we observe no clearly resolved peak in the $^{25}$Mg-gated, $^{26}$Mg-gated, or summed spectrum. However, the data are not well described by a fit that does not include a peak in this region. For a conservative treatment of states in this region, we use the results of the multiple-Gaussian fit described in Section~\ref{sec:1132} to extract an upper limit on the cross section, and hence $S_\alpha$, for a hypothetical state in this energy regime.
Specifically, we use the amplitude of the ${\sim} 11.17$~MeV peak in the $^{25}$Mg-gated spectrum to set a $90\%$ confidence level (CL) upper limit on the ${}^{22}\mathrm{Ne}({}^6\mathrm{Li}, dn){}^{25}\mathrm{Mg}$ cross section for \emph{any one} state between 11.17--11.25~MeV. We then use this cross section to calculate  upper limits on the $({}^6\mathrm{Li}, dn)$ cross section for each of the four natural-parity states identified in Ref~\cite{Massimi2017} ($E_x = 11.112$, $11.163$, $11.169$, and $11.171~$MeV). For this, we assume that $100\%$ of the observed upper-limit strength goes into each state individually. This results in a conservative upper limit because if the strength were shared between one or more states, the resulting cross sections would be lower for each.
}

From the upper limits on the ${}^{22}\mathrm{Ne}({}^6\mathrm{Li}, dn){}^{25}\mathrm{Mg}$ cross sections, we calculate upper limits on $S_\alpha \Gamma_{n} / \Gamma$ by normalizing to the presently-observed $S_\alpha$ for the $E_x=11.32$~MeV resonance, which is in turn normalized to $\omega\gamma^{\mathrm(11.32)}_{(\alpha,\gamma)}$. We take the $J^\pi$ for each of the four lower-energy resonances from Refs.~\cite{Massimi2012, Massimi2017} and do separate normalizations for both the $0^+$ and $1^-$ assignments to the $E_x=11.32$~MeV resonance. We convert these into limits on $S_\alpha$ by multiplying by $\Gamma/\Gamma_n$, taking $\Gamma_n$ and $\Gamma_\gamma$ from Ref.~\cite{Massimi2017} (and assuming $\Gamma \simeq \Gamma_n + \Gamma_\gamma$).
For the $E_x=11.171$~MeV resonance, which has a significant $\gamma$-ray decay branch and a large uncertainty on the neutron width, we adopt $\Gamma_n/\Gamma = 1/6$
for these calculations, i.e.\ the smallest value consistent with Ref.~\cite{Massimi2017}. This gives a conservative upper limit on $S_\alpha$ since a smaller $\Gamma_n/\Gamma_\gamma$ results in a larger $S_\alpha$ using the present procedure.
The resulting upper limits are presented in Table~\ref{tab:Table2}, along with a summary of the resonance parameters adopted for the $E_x = 11.32$~MeV state.

The $\gamma$-decaying resonance at $E_x=11.171$~MeV  is the likely candidate for the strong  $\alpha$ cluster state with $J^\pi = (1^-, 2^+)$ reported by Talwar \emph{et al}.\ \cite{Talwar2016}. Our upper limit on the spectroscopic factor for this state is substantially below that reported in Ref.~\cite{Talwar2016}, even when the latter is re-normalized to the present $\omega\gamma_{tot}^{(11.32)}$.
An even more stringent upper limit of $\Gamma_\alpha^{(J=2)} < 1.3\ee{-11}~$eV is reported in the concurrent sub-Coulomb study, Ref.~\cite{Jayatissa2019}.
A possible reason for the discrepancy between Ref.~\cite{Talwar2016} and the present experiment (along with Refs.~\cite{Giesen1993, Jayatissa2019}) is that the state observed in Ref.~\cite{Talwar2016} is actually a higher-spin state ($J \geq 3$) and thus more likely to be populated with their beam energy of $E^{(\mathrm{lab})}_{{}^6\mathrm{Li}} = 82.3$~MeV. This would also be consistent with a very recent GAMMASPHERE measurement which observed $\gamma$-ray decay from a state at $E_x=11.171$~MeV to a $4^+$ level, indicating a spin ranging from $2$--$6$ \cite{Lotay2019}.

\section{Astrophysical Implications}

\begin{figure}
\centering
	\includegraphics[width=8cm]{mc-rates-longland.pdf
	\caption{Updated ${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ (top) and ${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ (bottom) reaction rates, presented as a ratio to the recommended rates given by Longland \emph{et al}., Ref.~\cite{Longland2012}. The red dashed line represents our recommended rate, while the surrounding band represents the extent between our low and high rates. Also included for comparison are the recommended rates (also given as ratios to Ref.~\cite{Longland2012}) from Talwar \emph{et al}.~\cite{Talwar2016} (solid blue curve labeled ``Talwar'' in the legend) and  the upper limits presented in Massimi \emph{et al}.~\cite{Massimi2017} (green dot-dashed curve labeled ``Massimi'').
\label{fig:Rates}
}
\end{figure}

\begin{figure}
\centering
	\includegraphics[width=8cm]{rates-arxiv.pdf}
	\caption{Fractional resonance contributions of individual resonances to the median ${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ (top) and ${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ (bottom)  rates.
	\label{fig:RatesCompare}
}
\end{figure}

\begin{table}
\centering
\footnotesize
\begin{threeparttable}
\caption{Resonance properties adpoted for the Monte Carlo rate calculations.\label{tab:RateProperties} }
\begin{tabular}{cccc}
\hline
$E_x$ & \multirow{2}{*}{$J^\pi$} & \multirow{2}{*}{$\Gamma_n/\Gamma_\gamma$} & $\Gamma_\alpha$ \\
(MeV) & & & (eV) \\ \hline
10.8226(30)\tnote{a} & $2^+$ \tnote{a} & $0$                   & $2.1 \pm 0.3\mathrm{(stat)} \pm 0.4 (\mathrm{sys})\ee {-22}$\tnote{d,g}\\
10.9491(8)\tnote{a}  & $1^-$ \tnote{a} & $0$                   & $3.0 \pm 0.3\mathrm{(stat)}{}^{+0.8}_{-0.6}(\mathrm{sys})\ee{-14}$\tnote{d,g} \\
11.0809(40)\tnote{a} & $2^+$ \tnote{a} & $0$                   & $5.7 \pm 0.7\mathrm{(stat)}{}^{+1.4}_{-1.2}(\mathrm{sys})\ee{-11}$\tnote{d,g} \\
11.112(6)\tnote{b}   & $2^+$\tnote{b} & $1530(67)$\tnote{b,e}  & $< 2.2\ee{-10}$\tnote{f} \\
11.163(2)\tnote{b}   & $2^+$\tnote{b} & $1896(137)$\tnote{b,e} & $< 1.3\ee{-11}$\tnote{d,h} \\
11.169(1)\tnote{b}   & $3^-$\tnote{b} & $588(36)$\tnote{b,e}   & $< 1.3\ee{-11}$\tnote{d,h} \\
11.171(1)\tnote{b}   & $2^+$\tnote{b} & $0.2$--$6$\tnote{b}    & $< 1.3\ee{-11}$\tnote{d,h} \\
11.3195(25)\tnote{c} & $0^+$\tnote{d} & $1.14(26)$\tnote{f}    & $7.9(13) \ee{-5}$\tnote{f} \\
\multirow{2}{*}{${>} 11.32$} & \multicolumn{3}{p{5.8cm}}{Resonance strengths and energies adopted from Ref.~\cite{Jaeger2001} for $(\alpha,n)$ and Ref.~\cite{Wolke1989} for $(\alpha,\gamma)$.} \\
\hline
\end{tabular}
		\begin{tablenotes}
			\item[a]{Adopted from Ref.~\cite{Lotay2019}.}
			\item[b]{Adopted from Ref.~\cite{Massimi2017}.}
			\item[c]{Adopted from Ref.~\cite{Hunt2019}.}
			\item[d]{Adopted from Ref.~\cite{Jayatissa2019}.}
			\item[e]{Treated as negligable in the $(\alpha,\gamma)$ rate calculation.}
			\item[f]{Adopted from the present work.}
			\item[g]{A common (correlated) systematic uncertainty of ${}^{+25\%}_{-21\%}$ has been generated for each of these resonances.}
			\item[h]{See text for a detailed explanation.}
		\end{tablenotes}
	\end{threeparttable}
\end{table}

To investigate the impact of our measurements on the stellar ${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ and ${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ reaction rates, we have calculated low, recommended, and high rates using a Monte-Carlo procedure similar to the one described in Ref.~\cite{Longland2010}. This procedure accounts for uncertainties in nuclear physics quantities by treating them as probability density functions (PDFs), randomly sampling each quantity from its presumed PDF over many trials (here we use $N=50,000$). The resulting distribution of reaction rates is then analyzed to extract the low ($15^{th}$ percentile), recommended ($50^{th}$ percentile), and high ($85^{th}$ percentile) rates.

The $(\alpha, n)$ calculations include contributions from the five resonances treated in the present work, along with resonances above $E_x = 11.32$~MeV. The $(\alpha, \gamma)$ calculations include the four resonances observed in Ref.~\cite{Jayatissa2019}, along with the $E_x=11.171$~MeV resonance and resonances above $11.32$~MeV. A detailed list of the adopted excitation energies, $n/\gamma$ branching ratios, and $\alpha$ partial widths, including the associated uncertainties, is given in Table~\ref{tab:RateProperties}. The states at $E_x = 11.163$, $11.169$, and $11.171$~MeV require special consideration, as the $11.163$ and $11.169$ states were not treated in Ref.~\cite{Jayatissa2019}. However, because they are so close in energy to the $11.171$~MeV state, the experimental cross section limit of $0.8~\mu$b/sr is actually the limit for the \emph{total} population of all three states. For a conservative treatment, we adopt individual upper limits of $\Gamma_\alpha < 1.3\ee{-11}$~eV for each of these three states. This limit is only correct for $J=2$ states; however the upper limit for the $3^-$ state at $E_x=11.169$~MeV  would be even lower, given the same experimental cross section. Hence the application of the $J = 2$ limit to this state is again conservative.

\begin{table}
\centering
\footnotesize
\caption{Monte Carlo rates calculated for the ${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$ and ${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$ reactions. The rates are presented as $\log_{10} \left( N_A \left\langle \sigma v \right\rangle \right)$, in units of cm$^3$/mol/s. \label{tab:Rates} }
\begin{tabular}{cccc|ccc}
 & \multicolumn{3}{c}{${}^{22}\mathrm{Ne}(\alpha,n){}^{25}\mathrm{Mg}$} &  \multicolumn{3}{c}{${}^{22}\mathrm{Ne}(\alpha,\gamma){}^{26}\mathrm{Mg}$}\\
\hline
 $T_9$    & Low & Median & High & Low & Median & High \\
\hline
0.10 & -- & -- & --             & -24.12 & -24.01 & -23.90   \\
0.11 & -- & -- & --             & -22.66 & -22.54 & -22.44   \\
0.12 & -25.96 & -24.89 & -24.32 & -21.44 & -21.32 & -21.21   \\
0.13 & -24.39 & -23.33 & -22.76 & -20.40 & -20.29 & -20.18   \\
0.14 & -23.02 & -22.00 & -21.43 & -19.51 & -19.39 & -19.29   \\
0.15 & -21.79 & -20.84 & -20.28 & -18.72 & -18.61 & -18.51   \\
0.16 & -20.63 & -19.82 & -19.27 & -18.01 & -17.91 & -17.82   \\
0.18 & -18.48 & -18.04 & -17.57 & -16.77 & -16.68 & -16.60   \\
0.20 & -16.66 & -16.45 & -16.14 & -15.68 & -15.60 & -15.53   \\
0.25 & -13.34 & -13.24 & -13.15 & -13.21 & -13.14 & -13.07   \\
0.30 & -11.11 & -11.02 & -10.94 & -11.13 & -11.05 & -10.97   \\
0.35 & -9.50 & -9.42 & -9.34    & -9.57 & -9.49 & -9.40      \\
0.40 & -8.28 & -8.20 & -8.13    & -8.40 & -8.31 & -8.22      \\
0.45 & -7.28 & -7.21 & -7.15    & -7.49 & -7.41 & -7.31      \\
0.50 & -6.40 & -6.36 & -6.31    & -6.77 & -6.69 & -6.59      \\
0.60 & -4.86 & -4.84 & -4.82    & -5.71 & -5.62 & -5.53      \\
0.70 & -3.59 & -3.58 & -3.56    & -4.95 & -4.86 & -4.78      \\
0.80 & -2.57 & -2.56 & -2.55    & -4.37 & -4.29 & -4.21      \\
0.90 & -1.75 & -1.74 & -1.72    & -3.89 & -3.82 & -3.75      \\
1 .00& -1.08 & -1.06 & -1.05    & -3.47 & -3.42 & -3.35      \\
\hline
\end{tabular}
\end{table}

\revised{
In Figure~\ref{fig:Rates}, the resulting low, recommended, and high rates are plotted as a ratio to the recommended rates given by Longland \emph{et al}.\ in Ref.~\cite{Longland2012}.
For comparison, we also show the ratio-to-Longland of the recommended rates given by \etal{Talwar} \cite{Talwar2016} and the upper limits of \etal{Massimi} \cite{Massimi2017}. Numerical values of our low, recommended, and high rates are also given in Table~\ref{tab:Rates}.
Figure~\ref{fig:RatesCompare} shows the individual contributions of each resonance to the overall rate. We find that for the ${}^{22}\mathrm{Ne}(\alpha, n){}^{25}\mathrm{Mg}$ reaction, the $E_x=11.32$~MeV resonance completely dominates the total rate in the  temperature regime from ${\sim} 0.2$--$0.4$~GK,  where ${}^{22}\mathrm{Ne}(\alpha,\linebreak[1] n){}^{25}\mathrm{Mg}$ is thought to be the primary neutron source in the He-core burning phases of AGB stars. The presently-established $(\alpha,n)$ strength of this resonance results in a recommended rate that is up to a factor  ${\sim} 3$ lower than Refs.~\cite{Talwar2016,Longland2012,Massimi2017} in the crucial temperature regime from 0.2--0.4~GK.
For $T>0.4$~GK, resonances above $E_x = 11.32$~MeV begin to contribute to the overall $(\alpha,n)$ rate, eventually becoming dominant for $T>0.6$~GK. Below $0.2$~GK, the $E_x = 11.112$~MeV resonance is potentially dominant. This resonance still carries large uncertainties on its $\alpha$ partial width, leading to the large uncertainty band for the overall rate in this temperature region. As a result, a crucial focus of future measurements should be establishing tighter limits on the $\alpha$ width of this resonance.
We note additionally that the resonances at $E_x = 11.163,$ $11.169$, and $11.171$ are nearly inconsequential to the overall rate---with a fractional contribution of ${\sim} 10^{-3}$ or less across the entire relevant temperature regime for the $s$-process. This conclusion is the result of the stringent upper limits set on the $\alpha$ partial width in Ref.~\cite{Jayatissa2019}.

 For the ${}^{22}\mathrm{Ne}(\alpha,\linebreak[1] \gamma){}^{26}\mathrm{Mg}$ reaction, the total rate is dominated below ${\sim} 0.2$~GK by the $10.823$ and $10.949$ resonances---whose strengths are now well characterized by Ref.~\cite{Jayatissa2019}. Between ${\sim} 0.2$--$0.25$~GK the $11.081$~keV resonance dominates, and again the strength of this resonance is now well characterized by Ref.~\cite{Jayatissa2019}.
Above ${\sim} 0.25$~GK, the $E_x = 11.32$~MeV resonance, with a well-established strength of 37(4)~$\mu$eV, dominates. As with the $(\alpha, n)$ rate, the $E_x = 11.171$~MeV resonance is completely inconsequential---less than a  $10^{-4}$ fractional contribution to the total rate over all temperatures. As a result, our recommended rate is substantially below Talwar \emph{et al.}\ (maximum factor ${\sim} 10$) up to ${\sim} 0.6$~GK. In contrast, the present rate is significantly above the \etal{Longland} recommended rate below 0.25~GK (maximum factor ${\sim} 45$). Below 0.2~GK, this is primarily the result of \etal{Longland} using an upper limit of $\Gamma_\alpha < 2.9\ee{-15}$~eV for the 10.949~MeV resonance, adopted from Ref.~\cite{Ulgade2007}. Subsequent to that publication, strengths at least an order of magnitude larger than this limit have been established by both Ref.~\cite{Talwar2016} and Ref.~\cite{Jayatissa2019}, leading to the much larger $(\alpha,\gamma)$ rate in this temperature regime presented both in the present work and in Ref.~\cite{Talwar2016}. Between 0.2--0.25~GK, the higher rate is mainly the result of Ref.~\cite{Longland2012} neglecting the 11.081~MeV resonance, whose contribution again was not established until Refs.~\cite{Talwar2016, Jayatissa2019}.

We emphasize that the rates presented here, and the corresponding conclusions, are dependent on the spin assignments adopted in Table~\ref{tab:RateProperties}. More conservative rate calculations, which account for uncertainties in the spin, can be found in Ref.~\cite{Jayatissa2019}.  The overall conclusions are not subtantially different between the two treatments.
}

\section{Summary}

In summary, we have measured the $^{22}\mathrm{Ne}({}^6\mathrm{Li}, d){}^{26}\mathrm{Mg}$ reaction in inverse kinematics, using a $^{22}\mathrm{Ne}$ beam with an energy of $154$~MeV. We detected both the outgoing $d$ and $^{25,26}$Mg in coincidence, which gives sensitivity to $n/\gamma$ branching ratios through recoil tagging. For the key $s$-process resonance at $E_x=11.32$~MeV, we find that $\Gamma_n/\Gamma_{\gamma} = 1.14(26)$, roughly a factor $3$ below the ratio established from direct measurements. Normalizing to the well-known $^{22}\mathrm{Ne}(\alpha, \gamma){}^{26}\mathrm{Mg}$ resonance strength, we establish a new $^{22}\mathrm{Ne}(\alpha, n){}^{25}\mathrm{Mg}$ strength of $42(11)~\mu$eV for the $E_x = 11.32$~MeV resonance.  The angular distributions for this state are consistent with $J^\pi=(0^+,1^-)$ spin-parity assignments, which agrees with Ref.~\cite{Jayatissa2019}.
We note that the presently-established strength is independent of spin assignments or optical model calculations and depends only on $\Gamma_n/\Gamma_\gamma$ and the well-established $\omega\gamma_{(\alpha,\gamma)}^{(11.32)}$.

For neutron-unbound resonances below $E_x = 11.32$~MeV, we have determined upper limits on $\omega\gamma_{(\alpha,n)}$ and $\omega\gamma_{(\alpha,\gamma)}$ by combining an analysis of our ${}^{22}\mathrm{Ne}({}^6\mathrm{Li}, dn){}^{25}\mathrm{Mg}$ specrum with the $\Gamma_n$ and $\Gamma_\gamma$ reported in Ref.~\cite{Massimi2017}. In all cases, our upper limits on the $(\alpha,n)$ strength are below the direct-measurement limit of $6\ee{-8}$~eV reported in Ref.~\cite{Jaeger2001}. However, more stringent limits for the resonances between $E_x = 11.163$--$11.171$~MeV are concurrently set in Ref.~\cite{Jayatissa2019}. As a result we adopt these more restrictive limits for subsequent rate calculations.

\revised{
The presently-established, reduced strength of the $E_x = \linebreak[1] 11.32$~MeV resonance results in a recommended $(\alpha,n)$ rate, calculated using a modern Monte Carlo procedure, that is significantly below Refs.~\cite{Talwar2016, Longland2012, Massimi2017} in the crucial temperature regime from $0.2$--$0.4$~GK. }
The resulting decrease in the neutron flux is expected to reduce predicted $s$-process abundances for elements above mass ${\sim} 60$; however, this is likely to be mitigated by the similar decrease in the $\mathrm{Ne}(\alpha, \gamma){}^{26}\mathrm{Mg}$ rate in the same temperature regime.
Detailed calculations evaluating the impact of the present changes in the recommended $\mathrm{Ne}(\alpha, n){}^{25}\mathrm{Mg}$ and $\mathrm{Ne}(\alpha, \gamma){}^{26}\mathrm{Mg}$ rates on $s$-process abundances will be presented in a forthcoming publication.

Taking the present results together with Ref.~\cite{Jayatissa2019}, we highlight two major, outstanding uncertainties surrounding the $^{22}\mathrm{Ne}(\alpha, \linebreak[1] n){}^{25}\mathrm{Mg}$ reaction rate. First, the $\alpha$ partial width of the $2^+$, $E_x =11.112$~MeV resonance reported by Massimi \emph{et al.}\ \cite{Massimi2017} is not well constrained. This resonance potentially dominates the overall rate below ${\sim} 0.2$~GK due to its low energy---only $19$~keV above the neutron threshold. As a result, the total reaction is not well constrained at low temperatures. Second, the substanial discrepancy between the present $\omega\gamma_{(\alpha,n)}^{(11.32)}$ and direct measurements clearly highlights a need for future direct $(\alpha, n)$ measurements, or complimentary indirect studies of this key resonance. In particular, direct measurements that reduce room background, either by being performed underground or above ground using inverse kinematics and a recoil separator, are particularly welcomed.

\section*{Acknowledgements}
We express our thanks to the technical staff at the Texas A\&M University Cyclotron Institute. Financial support for this work was provided by the US Department of Energy, Office of Science, award No.\ DE-FG02-93ER4077; the US National Nuclear Security Administration, award No.\ DE-NA0003841, and the Nuclear Solutions Institute at Texas A\&M University. J.A.T., W.N.C., and G.L.\ acknowledge support from the Science and Technology Facilities Council (U.K.) Grant No.\ ST/L005743/1.  The ${}^{6}\mathrm{LiF}$ targets were provided by the Center for Accelerator Target Science at Argonne National Laboratory.

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