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Bill Hader to Develop Series for HBO
HBO has signed former Saturday Night Live cast member Bill Hader to an exclusive development deal to create and star in a new series for the network.
It is not yet known whether Hader will develop a half-hour or hour-long series.
Hader was a member of the SNL cast from 2005 to 2013. He was nominated in 2012 for an Emmy for supporting actor in a comedy series for his work on the show.
News of the deal was first reported by Deadline.

subset: commoncrawl


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Even as Race 3 is all set to cross Rs 150 crore in a week, here's the first week box office collection of last five Salman Khan films.
Salman Khan starrer Race 3 released on June 15 and made the most out of the festival weekend in terms of box office collections. The film opened at Rs 29.17 crore and became the highest Hindi film opener of 2018. The film has been earning big bucks at the box office since then. In the first six days, Race 3 has earned Rs 142.01 crore and it looks like the film will cross the Rs 150 crore mark on its seventh day. With no big Hindi film releases this Friday, the Salman Khan starrer will possibly continue its glorious run at the box office in the second week as well.
Here's what Salman Khan's last five films made at the box office in the first week.
1. Tiger Zinda Hai – Rs 206.04 crore
This 2017 Salman Khan and Katrina Kaif film was a massive hit. Directed by Ali Abbas Zafar, this film was action packed and saw Salman playing Tiger after the much popular Ek Tha Tiger. In the first week, the film managed to earn Rs 206.04 crore.
2. Tubelight – Rs 106.86 crore
Tubelight was a disappointment for Salman Khan fans. This Kabir Khan directorial managed to earn Rs 106.86 crore in the first week but the collection drastically after the first week.
3. Sultan – Rs 229.16 crore
Starring Salman Khan and Anushka Sharma, this sports drama had Salman playing the character of a Haryanvi wrestler. Directed by Ali Abbas Zafar, the film earned Rs 229.16 crore in the first week.
4. Prem Ratan Dhan Payo – Rs 172.82 crore
Salman collaborated with Sooraj Barjatya after Hum Saath Saath Hain and this reunion drew many fans to theatres. Also starring S2onam Kapoor, this family drama earned Rs 172.82 crore in the first week.
5. Bajrangi Bhaijaan – Rs 184.62 crore
Loved by fans and critics alike, this Salman Khan film was even loved by his staunch haters. In the first week, this Kabir Khan directorial earned Rs 184.62 crore.
Race 3 box office collection: The Salman Khan starrer inches towards Rs 200 crore mark worldwide
Race 3, Padmaavat and Baaghi 2 in Top 5 weekend openers of 2018 list
Source: Read Full Article


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Need something to get your sewjo running? Make a fun headscarf below.
Have you been wanting to make a Rita Blouse? I have a simple tutorial here on how I made mine.
Maybe it's been awhile since you cleaned your sewing machine, get that beauty running smoothly in just a few easy steps.
What does your sewing or crafting space look like? Mine has been a work in progress. Here are a couple of photos of my sewing space. It's nothing to write home about, yet. But, it's getting there.
Thanks for dropping by! Visit again soon and next time, bring snacks.
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You will now be taken to Amazon to complete your purchase.purchase in a new tab
***Update***Thursday 01/30/2020 Brigitte is back home and recovering from her surgery! Surgery went well, it was a smooth process with the Surgeon. He was able to keep all of her kneecap and repair it with screws and wiring. Depending on how Brigitte's body responds, there could be a second surgery to remove the wires once the bone is solidly healed. She will have a post-op appointment within the next two weeks, and we will find out more with timeframes for physical therapy. There is a long road ahead still, and we are so grateful to finally be on this step! We will continue to post updates on her progress as she has followup appointments, physical therapy appointments, and when she will be back to the shop!! We honestly cannot thank all of you enough!!! Thank you for holding the space for her (and us) during this time. We are so so so grateful for your financial contributions so we could get this surgery done for Brigitte. Thank you all for thoughts, prayers, meals, cards, flowers, goodies, texts, messages, calls, and check ins. We are feeling the love of from all of you, Thank you ❤ With Love, Noelle (Brigitte and Doug's Daughter) Ways to help right now: Meal Coverage and Donations If we can take prepping and cooking dinners off their plate, it would be wonderful! See details below for dietary requests. If you are local please sign up for a date to bring a meal to the shop: Brigitte's Serenity Studio 1513 Grass Valley Hwy. Auburn, Ca 95603 Drop off anytime in the window of 3pm-6pm *if you need a different time just message me texts are best right now (530)305-4431* If you are far away and want to contribute please consider digital gift cards for restaurants like: Chipotle, Mod Pizza, or Garden of Eatin' or use the Paypal link. (incase there is any link trouble the email is: [email protected]) Donations: I know there will be many unforeseen financial pressures that will arise as Brigitte does not have medical insurance and will be out of work for several months. They will be down to a very bare income, as Brigitte will not be able to collect unemployment/disability during her healing. If you are able to please donate, or come by and shop at the studio. They will be so grateful for the support. (incase there is any link trouble the email is: [email protected]) Thank you for taking the time to check this out, and thank you for your love and support to both Brigitte and Doug as they navigate this. In love and light, Noelle
Brigitte is a Vegetarian and Gluten Free. Please keep any sauces, stocks/broths, etc. a veggie base and gluten free. She loves veggie packed salads.


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FRIDAY FODDER: York knows nothing about winning in the NFL
For the Nevada Apeal
Sports fodder for a Friday morning … Does anybody outside the DeBartolo or York family tree actually believe Jed York will return the San Francisco 49ers to their glory years?
York is just a spoiled little rich kid who simply gets bored when he doesn't get everything he wants. He got bored with coach Mike Singletary this week after just two full seasons and fired him.
York, who only runs the 49ers because his mommy's brother is former 49ers owner Eddie DeBartolo, obviously knows nothing about football. Building a winning NFL organization takes patience, another subject little Jed knows nothing about. But that's nothing new in the DeBartolo family. Uncle Eddie, another former rich kid, also didn't know a thing about football or patience. He merely stumbled upon Bill Walsh in 1979 and lived off that stroke of luck for 20 years. Maybe Jed will get lucky this time, too, as he looks for another general manager and head coach. Don't count on it.
The 49ers should do everything in their power to lure Mike Holmgren away from the Cleveland Browns. Holmgren would be perfect for the 49ers.
He could serve as team president (the role he currently has in Cleveland), general manager and head coach. He would return the glory years to the 49ers. Holmgren, who was born in San Francisco and cut his NFL coaching teeth under Bill Walsh with the 49ers, would win a Super Bowl with the 49ers. No question. The only question is whether little Jed would relinquish the keys to his favorite toy (the Niners). Don't count on it.
The biggest sports moment of 2010 in Northern Nevada?
That's an easy one. Wolf Pack 34, Boise State 31 on Nov. 26. It's the biggest Wolf Pack moment, football or otherwise, in school history, let alone the last 12 months. The Wolf Pack football team also owns the second biggest sports moment in Northern Nevada in 2010. Wolf Pack 52, California 31 on Sept. 17.
Now that Jim Rice is in the Hall of Fame with his 382 career homers, 2,452 hits, .298 lifetime average and 1,451 RBI, you also have to give serious consideration to Harold Baines (2,866 hits, 384 homers, 1,628 RBI, .289 average), Dave Parker (2,712 hits, .290 average, 339 homers, 1,493 RBI), Larry Walker (2,160 hits, .313 average, 383 homers, 1,311 RBI), Edgar Martinez (2,247 hits, 309 homers, 1,261 RBI, .312 average), Juan Gonzalez (434 homers, 1,404 hits, .295 average), Fred McGriff (493 homers, 1,550 RBI, 2,490 hits, .284 average) and about two dozen other players down through history. Rice is in the Hall for one reason: He played for the Boston Red Sox and used to pound the New York Yankees.
Jeff Bagwell is eligible for the Hall of Fame this year for the first time. It might be a good idea for the voters to hold off voting for him for a while. Did Bagwell use performance enhancing drugs or didn't he? Yes, he supposedly never failed a drug test. But we also know that a ton of guys who never failed a drug test actually did use performance enhancing drugs. Do you just penalize the guys who admitted cheating or got caught? Is that fair? Bagwell's body certainly ballooned to lumberjack proportions in his career. And, like most PED users, he was constantly injured in his later years. His numbers (449 homers, 1,529 RBI, 2,314 hits) are good but he's not a certain Hall of Famer even if he didn't cheat. He wouldn't get my Hall of Fame vote this year.
College basketball rosters have more turnover from one year to the next than a NBA D-League roster. The Wolf Pack men's basketball team will only lose two seniors (Illiwa Baldwin, Adam Carp) off of this year's team heading into the 2011-12 season.
But don't be shocked if Baldwin and Carp are not the only players who leave the program before next year. Sophomores Keith Olson (who can't seem to get healthy) and Marko Cukic and Patrick Nyeko (who can't seem to get off the bench) might also decide to move on.
The Pack also has six freshman on this year's team and some of them might decide that they'll likely have a better future somewhere else. The next 10 weeks will be very interesting at Lawlor Events Center.


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Bavarian Pretzel Sticks
House made soft pretzel sticks served warm with house made beer cheese 8.99
Peppered calamari strips served with house made pub sauce 11.99
Pork Cracklins
Pork rinds made fresh with choice of seasoning cajun, salt + pepper, garlic or ranch 5.75 Add queso 1.00
Spinach Artichoke Dip
Served hot with our fresh tortilla chips
Jalapenos upon request 13.99
Hummus Plate
House made red pepper hummus served with warm flatbread, vegetables, roasted feta, roasted garlic + kalamata olives 11.99
Naked Chicken Wings
Choice of house made bbq sauce, traditional, sweet + spicy, honey garlic zing 12.99
Served with salsa and guacamole 7.99
Add chicken 4
House Made Kettle Chips
House made kettle potato chips served with sour cream bacon dip 6.00
Cheese Curds
Cheese curds fried to a golden brown 10.99
Tortilla Chips and Salsa
Fresh cut corn tortilla chips served with house made salsa and guacamole 7.99 Add queso 1.00
Onion Rings
Served with house made pub sauce 6.50
Soup & Salad
Chowder or soup of the day
Cup 4.99 / Bowl 7.99 / Sourdough Bowl 9.99
Soup + Salad Combo
Cup 9.99 / Bowl 12.99 / Sourdough Bowl 14.99
Quinoa Power Bowl
Quinoa, red peppers, red onion, kale, mix cheese, black bean, pistachio nut, in house pickled egg, avocado 10.99
The Wedge (Try it grilled!)
Roma crunch topped with bleu cheese dressing + crumbles, green onion, bacon bits + grape tomatoes 11.99 ½ wedge 5.99
Spring Mix Salad
Spring mix blend topped with carrots, grape tomatoes, crispy beet matchsticks + cucumber 8.99
NW Roasted Beet Salad
Oven roasted red beets, dried cranberries, walnuts, pickled onions + roasted feta cheese, served on a bed of mixed greens 14.99 ½ beet salad 7.49
Recommend Apple Vinaigrette Dressing
Crispy Buffalo Chicken Salad
Crispy chicken tenders tossed in traditional buffalo sauce, grape tomatoes + cucumber, served on a bed of mixed greens 14.99
Recommend Bleu Cheese Dressing
Chef Salad
Turkey, ham, jack cheddar, tomato, bacon bits + hard-boiled egg, served on a bed of mixed greens 14.99
Caesar Salad
Caesar dressing over lettuce with parmesan, cracked pepper + croutons 10.99
(Add chicken to any salad – 4)
Chicken Caprese Panini
Grilled Chicken breast, fresh mozzarella, tomato, fresh basil, Spinach + balsamic reduction on ciabatta 10.99
Veggie Wrap
Hummus, red onion, chopped romaine, spinach, fresh red pepper, micro greens, avocado, feta +tzatziki and tortilla 9.99
Lamb Wrap
Seasoned lamb patty, kalamata olives, feta, spinach, tomato, red onion, cucumber + tzatziki 15.99
Smoked Tuna Melt
Ahi Tuna smoked in house on cedar planks with lightly smoked gouda + bacon
Served on peppered sourdough bread 13.99
Mill City Reuben
Corned beef sliced with swiss cheese, sauerkraut + 1000 Island
Served on marble rye 13.99
Club House Sandwich
Turkey, ham, bacon, swiss cheese, white cheddar cheese with lettuce, tomato, red onion + mayo
Served on toasted sourdough bread 15.99
French Dip
Roast beef, sautéed mushrooms, grilled onions, horseradish + smoked gouda cheese
Served on a ciabatta roll 14.99
Turkey Bacon Panini
Smoked turkey, white cheddar cheese, peppered bacon, pickled onion, spinach + chipotle aioli
Served on sourdough bread 13.99 add Avocado 2.00
Bacon with fried egg, lettuce, tomato + mayo
Served on toasted sourdough bread 10.99
Triple Grilled Cheese + Cup of soup
Gouda, Pepper jack + White Cheddar 9.99
Deli Sandwich
Served with lettuce, tomato, onion, mayo +stoneground mustard 10.99
½ sandwich with a cup of soup or salad 8.99
Choice of bread: sourdough or marble rye
Choice of meat: smoked turkey, ham or corned beef
Choice of cheese: white cheddar or swiss
(Gluten free bread available – 4)
All burgers served with lettuce, tomato, and onion. Mayo upon request.
*Consumer advisory: Consuming raw or undercooked meats or eggs may increase your risk of food borne illness
Vegetarian Quinoa Patties Available
Gluten Free Buns 4
98607 Burger*
Ham, peppered bacon, white cheddar, fried egg, lettuce, tomato, red onion + mayo 15.99
Smoked Blue Onion Bacon Burger*
Smoked bleu cheese crumbles, beer battered onion rings, bacon, lettuce + tomato 13.99
Rauch BBQ Bacon Burger*
Peppered bacon, house made bbq sauce, white cheddar, lettuce, tomato, red onion + horseradish aioli 13.99
Mt. Hood Burger*
Sautéed mushrooms, grilled onions piled high + swiss cheese 12.99
Guacamole Bacon Burger*
Guacamole, peppered bacon, pepper jack cheese, lettuce, tomato + red onion 15.99
Crispy Buffalo Chicken Burger
Crispy chicken tender tossed in traditional buffalo sauce with bleu cheese dressing + crumbles, lettuce, tomato + red onion (grilled chicken upon request) 12.99
Portabella Burger
Portabella mushroom marinated in a balsamic seasoned reduction with garlic dill goat cheese, spinach, tomato + red onion 13.99
Quinoa Burger
Made with mushrooms, black beans, quinoa, onion, peppers, corn, jack cheddar + oatmeal, lettuce, tomato + red onion 11.99
½ pound beef patty with lettuce, tomato + red onion 10.99
Add cheese for 1.50
(Gluten free bun available – 4)
Entree's & Pastas
3 Smoked Wild Hog Wings
Tossed in honey garlic glaze with roasted garlic mashed potatoes + your choice of one side: steamed veggie, ½ order plan ol' mac, kale cole slaw or side salad 18.99
Fish + Chips
In house beer battered rockfish, served with fries, coleslaw + tartar sauce 15.99
Clam Strips & Shrimp Basket
Shrimp + clam strips, served with fries, coleslaw, tartar + cocktail sauce 16.99
Chicken Strip Basket
Crispy chicken tenders + fries
Try with our in house bbq sauce, buffalo sauce, sweet & spicy or honey garlic zing 12.99
Mill City Mac + Cheese
Shell pasta with italian sausage, tomato, mushroom in house made beer cheese, topped with colby jack cheese + crispy garlic chips 12.99
Chicken Alfredo Florentine
Shell pasta with chicken breast + spinach in a parmesan alfredo 13.99
Santa Fe Mac
Shell pasta, queso beer cheese, black bean, diced chicken, green chili, roasted corn,+ topped with green onion, cilantro and cotija cheese 13.99
Plain Ol' Mac
Shell pasta tossed in beer cheese, topped with colby jack cheese + crispy garlic chips 9.99
Add bacon 2.00 Add chicken 4.00
Beer Mac 6.00
Steamed Veggies 4.00
Kale cole slaw 4.00
French fries 4.50
Garlic fries 6.00
Tater tots 5.50
Sweet potato fries 5.50
Mill City Jr. Menu
(10 & Under)
Choice of side salad, fries or carrots w/ranch and a drink.
Choose ONE of the following options :
Chicken Fingers Basket
Cheeseburger Basket
Grilled Cheese
Kid Size Plain Mac
Flatbread Pizza Cheese or Pepperoni
Choice of side:
Fries, Carrots w/ranch, Side Salad
Drink Choice:
Apple Juice, Milk, Chocolate Milk, or Soda
Yukon Jack Bread Pudding $8.75
Cinnamon Bread Pudding and Custard with a Yukon Jack Sauce, Candied Pecans, Cranberry Raisins and Whipped Cream.
Choclate Brownie $8.75
Made with our Fromudder Stout served with ice cream.
Ice Cream Sundae $6.00
Two Scoops of Ice Cream with Chocolate Syrup, Candied Pecans, Whipped Cream and a Maraschino Cherry.
Root Beer Float $5.75
Barq's Root Beer with Two Scoops of Ice Cream
Beer Float $8.75
(21 and Over)
A pint of Beer and two scoops of Ice Cream
Recommended: Chocolate Porter or Trip Wire
Coke, Diet Coke, Sprite, Barq's Root Beer, Ginger Ale, Lemonade or Gold Peak Iced tea.
Paper Tiger's Las Delicious coffee.
Assorted Hot tea.
French Fries $5
Garlic Fries $6
Sweet Potato Tots $6
Pork Cracklin's $5
Kale Coleslaw $5
Side Salad $5
Vegetables $5
Cup of Soup $6


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Pet Names and What's the Most Popular Pet Names and Presidential Pet Names
Which Presidential Surname's Most Popular For Pets?
Photo 7 of 11
4. Hoover
I know I'm not the only one who describes my dog's eating habits as hoovering! Whether it came from the vacuums or this man himself, there are 36 registered pets that have it.
0previous images
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Jeff Mizanskey, Sentenced To Life In Prison For Marijuana, Released From Missouri Prison Tomorrow
Tomorrow is going to be a very, very big day. Jeff Mizanskey has been serving a life sentence in prison for non-violent marijuana only offenses in Missouri for over two decades. The Show-Me Cannabis campaign has been working very hard with the Mizanskey family to bring awareness to Jeff Mizanskey's case, and to work for Jeff's release. After a very long battle, Missouri's Governor granted clemency to Jeff Mizanskey, which led to a successful parole hearing. All of that culminates with Jeff's release tomorrow.
Tomorrow between 8 a.m. and 10 a.m. Jeff Mizanskey will walk out of the Jefferson City Correctional Center a free man. The petition that received almost 400k signatures was a success. Multiple YouTube videos calling for Jeff's release worked. Letters from 126 Missouri lawmakers to the Governor worked. All of the billboards, all of the Facebook shares, and everything else that activists have done has worked, proven by Jeff Mizanskey's release tomorrow.
I tip my hat to the Show-Me Cannabis campaign and to Jeff Mizanskey's family for all of the good work they have done, and a huge kudos to all of the other people that have helped fight for Jeff's freedom. I'm very curious to see what Jeff does next. It's my understanding that there will be a press conference and/or press release after Jeff is freed, and I'll make sure to post footage from that when I receive it. For now, check out Jeff's case from the information below:
- My dad is serving life without parole for marijuana
- Timeline of events from Mizanskey's lawyer, Dan Viets.
- 130 lawmakers ask for Mizanskey to be freed
- Petition for clemency
- A plea for clemency from the prosecutor who put him away.
- A documentary about Mizanskey's plight.
- The "prior and persistent drug offender" law Mizanskey was sentenced under has been repealed effective 2017.


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Week #12 2019
- Lettuce
- Kale
- Broccoli or cabbage
- Zucchini
- Sugar snap peas or green beans
- Kohlrabi
- Garlic
- Purplette bunching onions
- Potatoes
- Basil
- Carrots or beets
- Purslane or parsley
Hey hey summer is on its way. We had a nice cool week, with rain that gave our crops fresh energy, but also helped the weed seed germinate. Now the battle is on! Pig weed, thistle, lambs' quarters, annual morning glory and so on. Our critter enemies are also on the hunt from above and below ground. Yikes, just writing this makes me itch to get out there and work.
We are having a lavender wand making lesson in the barn today from 2-4. This is a wonderful way to keep the smell of lavender in your home all year. Member Janette Gill is very crafty and a good teacher and will lead us through this activity. I have tons of lavender from my mother's yard all ready for you to use.
Holiday week means a regular schedule for us, we will harvest Wednesday and have it ready for pick up by 1:00. If you are heading out of town, consider stopping by the farm before you go to make sure your trip includes fresh vegetables! Pick up eggs, cheese and beef as well. Maybe some flowers for that host of the party you are going to??
This may be the last week of sugar snaps. We are heading into beans and then cherry tomatoes. If you have not signed up to help yet, please do consider. We need all hands-on deck to get the harvest done. If the day you want to harvest is already booked, consider coming anyway. We can always find something for you to do. We understand not everyone can help harvest or wants to and that is fine.
Important dates to mark on your calendar:
- TBA – Finquita farm to table dinner put on by Alaskan chef apprentice Cole Roberts ("kohlrabi")
- August 25th – annual canning party !! 9 – 5
- September 22nd – PACSAC benefit farm to table dinner at La Finquita
- September 27th – "Prospera" benefit for Virginia Garcia Memorial Health Center, join me at my tables, all funds go to support health care for the most vulnerable in Washington County.
- October 6th – Harvest Festival
Here are some recipes for this week:
Crunchy Red Devils recipe by A. Doncsecz, Vegetarian Gourmet
2 Tablespoons Apple Cider Vinegar
2 shallots, minced
1/4 cup hot red pepper sauce
1 teaspoon grainy mustard
½ teaspoon sugar
3 medium kohlrabi bulbs
Whisk together all ingredients except kohlrabi with ½ cup water. Peel and thinly slice kohlrabi; stir into marinade, coating evenly. Cover and refrigerate 2-3 days, stirring occasionally. Serve cold or at room temperature.
Stir-Fried Kohlrabi from The Goodness of Potatoes and Root Vegetables
3 kohlrabi, peeled
3 medium carrots
4 tablespoons peanut or safflower oil
3 cloves garlic, peeled and thinly sliced
1 inch piece gingerroot, peeled and thinly sliced
3 green onions, sliced
1-2 fresh chili peppers, sliced, optional
4 tablespoons oyster sauce (optional)
3 teaspoons sesame oil & soy sauce, each
Slice kohlrabi and carrots into thin ovals. Heat oil in large heavy skillet; when it begins to smoke, toss in garlic and ginger. Stir once then add kohlrabi and carrots; toss and cook 2 minutes. Add green onions and chilies; stir-fry 1 minute, then pour in ½ cup water. Cover, reduce heat and cook 5 minutes. Remove cover and toss in a little salt and the sesame and soy, and oyster if using. Serve with rice.
Kohlrabi Pickle Chips from the Victory Garden Cookbook
1-2 pounds smallish kohlrabi, trimmed
3 small onions
1/4 cup pickling salt
2 cups vinegar
2/3 cup sugar
1 Tablespoon mustard seeds
1 teaspoon celery seeds
1/4 teaspoon tumeric
Peel and thinly slice kohlrabi and onions. Mix salt with 1 quart ice water, pour over the vegetables, and soak for 3 hours. Drain, rinse, and place in a bowl. Bring remaining ingredients to a boil, cook for 3 minutes, and pour over the vegetables. Cool, cover and refrigerate for 3 days
New Potatoes with garlic and parsley
READY IN: 38mins SERVES: 4
INGREDIENTS Nutrition
12 small red potatoes
4 garlic cloves, minced
2 tablespoons chopped fresh parsley
3 teaspoons lite olive oil (divided)
salt and pepper
Scrub the potatoes well.
Pare a 3/4″ strip around the middle of each potato (this is just to give you a little contrast in color).
Place potatoes in a saucepan, cover with water and bring to a boil.
Simmer covered for about 20 minutes or until tender.
Drain potatoes and place them in a bowl add two teaspoons of oil& toss.
In a nonstick frypan add the remaining oil over medium heat.
Add garlic, cook approximately 1 minute.
Add parsley, salt& pepper, mix well.
Add potatoes, reduce heat to low and cook stirring constantly for 1 or 2 minutes.


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Home > Research > Centers and Labs > DCIC
Digital Curation Innovation Center (DCIC)
About Us
The DCIC is an iSchool research center that explores how to integrate archived information with new data and how to better access these records to foster historical research engagement. Additionally, at the DCIC, faculty and students are developing interdisciplinary public, industry, and government partnerships to increase integration and access to big data and archival records and databases.
The DCIC provides iSchool students with the opportunity to work on research projects that address real archival and information management challenges faced by organizations including government agencies, academic institutions, and corporations.
Assistant Professor
PhD Student
Adjunct Lecturer
Senior Lecturer
Associate Professor
Lecturer & Career Services Lead
Associate Professor & Doctoral Program Director
Professor & Dean Emerita


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Analytics Consultant, Wells Fargo Advisors
John Miller is an Analytics Consultant at Wells Fargo Advisors in St. Louis, MO. John works on the Advice and Research Strategy Team where his group is responsible for client portfolio analytics. John has been with the firm for 5 years holding various analytics roles. Tableau is something that is a daily part of his team's role, from daily metric reports published to the team's server, to deep dive analytics to help Financial Advisors uncover opportunities to better serve their clients.


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1332 West Bryn Mawr Avenue, Chicago, IL - $900,000
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M.-R. L. Cioni1 - J. A. D. L. Blommaert2 - M. A. T. Groenewegen2 - H. J. Habing3 - J. Hron4 - F. Kerschbaum4 - C. Loup5 - A. Omont5 - J. Th. van Loon9 - P. A. Whitelock7 - A. A. Zijlstra8
1 - European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
2 - Institute of Astronomy, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
3 - Sterrewacht Leiden, Niels Bohrweg 2, 2333 RA Leiden, The Netherlands
4 - Institut für Astronomie der Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria
5 - Institute d'Astrophysique de Paris, CNRS, 98bis Bld. Arago, 75014 Paris, France
6 - Astrophysics Group, School of Chemistry and Physics, Keele University, Staffordshire ST5 5BG, UK
7 - South African Astronomical Observatory, PO Box 9, 7935 Observatory, Republic of South Africa
8 - Department of Physics, UMIST, PO Box 88, Manchester M60 1QD, UK
Received 8 January 2003/ Accepted 18 April 2003
This article presents the study of the light-curves extracted from the MACHO database of a sample of stars observed by the Infrared Space Observatory in the Small Magellanic Cloud. These stars belong to the ISO-Mini-Survey catalogue of the Magellanic Clouds (ISO-MCMS, Loup et al. in preparation). Most of them are in the asymptotic giant branch (AGB) and supergiant phases. The dominant period and amplitude of pulsation have been derived and the stars have been classified as Mira or Semi-Regular pulsators. Furthermore, the cross-identification with near-infrared DENIS and 2MASS magnitudes available within the ISO-MCMS allowed us: (i) to investigate the properties of these stars in the combined near- and mid-infrared colour-magnitude diagrams, (ii) to derive the bolometric magnitude by integrating the spectral energy distribution and (iii) to estimate the mass-loss rate. The stars have been divided into carbon- (C-) and oxygen-rich (O-rich) using the (J-KS, KS) colour-magnitude diagram and their period and amplitude distributions have been compared. C-rich AGB stars have a sharp peak in their period distribution at about 250 days and have on average a larger amplitude than O-rich AGB stars. This effect, not previously detected from the study of similar stars in the Large Magellanic Cloud and in the Baade's window, might be closely related to the metallicity of the environment in which the stars have formed.
Key words: galaxies: Magellanic Clouds - infrared: galaxies - stars: mass loss - stars: variables: general
In order to study the evolved AGB population it is thus important to utilize observations that cover the spectral range from the optical (I band) to the mid-IR. It is then possible to derive fundamental quantities such as the bolometric magnitude and the mass-loss rate of the stars. In addition, from the period, the amplitude and the regularity of the variation, it is possible to characterise the stars as Mira or Semi-Regular (SR) pulsators and to indicate, from the PLR, the mass of the stellar progenitor. In this article the properties of a sample of AGB stars in the SMC extracted from the ISO-Mini-Survey catalogue of the Magellanic Clouds (ISO-MCMS, Loup et al. in preparation), which already contains the cross-identification with the near-IR catalogues DENIS and 2MASS, are discussed. This is done by additionally analysing the light-curves extracted from the MACHO database. A similar work was performed in the LMC bar-west field (Cioni et al. 2001) and will be further extended to other fields where ISO measurements are now available. A detailed comparison of more or less obscured AGB variables between the two Clouds and the Baade's window NGC 6522 will be given in another paper (Glass et al. in preparation).
The data and the cross-identification with the light-curves are described in Sect. 2. In Sect. 3 the analysis of the period and amplitude of variability and the determination of the bolometric magnitude is presented. A discussion of the different type and variability class of the sources in the PLRs and in the near- and mid-IR colour-magnitude diagrams is given in Sect. 4. Section 5 concludes the article. Appendix A discusses the re-analysis of the LPVs studied by Feast et al. (1989) and B compares the bolometric correction obtained in this work with the relations by Alvarez et al. (2000) and Montegriffo et al. (1998).
The sample of data in the SMC, analysed here, is based on the cross-identification between the ISO-MCMS (Loup et al. in preparation), and the MACHO light-curves publicly available.
The ISO mini-survey in the direction of the SMC covers an area of 0.28 square degrees. Observations were performed with the infrared camera ISOCAM on board the ISO satellite in the LW2 (m) and LW10 ( m) wavebands. The catalogue lists 1333 sources brighter than about 12.4 and 11.3 mag in LW2 and LW10, respectively. The coordinates of the ISO sources are better than 4 with a faint tail up to 6 . The catalogue also lists the cross-identification with the near-infrared catalogues 2MASS (2nd Incremental Release PSC) and the DENIS (Epchtein et al. 1997) catalogue towards the Magellanic Clouds (DCMC - Cioni et al. 2000a), and a few smaller optical catalogues of carbon stars, HII regions, PNe and emission-line stars. According to the association likelihood criteria defined by Loup et al. (in preparation) 48% of the sources have no, or an unlikely, association with DENIS/2MASS; 13% have a questionable association; 25% have a confident association and the remaining 14% are "known'' sources with a DENIS/2MASS and optical counterpart. It is perhaps surprising that there are many ISO sources without a near-infrared counterpart. However, most of these sources are among the faintest ISO detections in both ISO wavebands. The histogram of their magnitudes and colour peaks at: LW2=12, LW10=11 and (LW2-LW10)=1.5. Moreover, the ISO-MCMS includes sources well detected in one band only. Among sources detected only in two bands about 86% have a near-IR counterpart. The ISO photometric magnitudes are part of the final version of the catalogue released to the Co-Is and associates in March 2002.
The MACHO (Alcock et al. 2000) light-curves were obtained from repeated measurements in two, blue and red, broad pass-bands from the 50 inch telescope at the Mount Stromlo Observatory in Australia. Observations of fields covering most of the Magellanic Clouds were performed from 1992 to 2000. The light-curves are easily accessible via the web interface giving in input the right ascension (RA) and the declination (DEC) of each source.
Figure 1 shows the regions observed by ISO superimposed on the MACHO fields. The area covered by ISO is entirely contained in MACHO fields number 211 and 212; a few sources are also present in field number 207. These MACHO fields were observed for the whole period of eight years while the observations of fields in the external parts of the SMC cover just five years. The OGLE light-curves cover a period of about five years (observations started in 1997). Because of the nature of LPVs, sources with periods from 100 to 1000 days, the MACHO light-curve database was preferred.
Each ISO source with a confident DENIS/2MASS association was searched for a light-curve in the MACHO database using, as input, the 2MASS coordinates. Variables were confidently identified within a radius of 1. Fig. 2 shows that most of the sources were actually associated within 1 . In a very few cases the MACHO counterpart, a source with a typical LPV light-curve, was not the closest to the 2MASS source - but still within no more than 4 . We consider a light-curve to be that of a LPV when a more or less periodic behaviour is detected by eye. It is expected that most of the sources detected in the near- and mid-IR are associated with AGB stars. This is a consequence of the mass-loss process occurring in AGB stars that builds up a circumstellar envelope observable in the mid-infrared.
Among the 502 sources with a confident DENIS/2MASS counterpart, 458have been found to have a MACHO light-curve. Table 1, available electronically at the CDS, lists the MACHO coordinates at the epoch J2000 (Cols. 1 and 2), the MACHO identifier field, tile and number (Cols. 3-5), the distance in arcsec between the 2MASS and the MACHO source (Col. 6) and the ISO-MCMS identifier (Col. 7). The first 10 lines are given as an example (Table 1).
The sources listed in Table 2 are those for which we could not find a convincing MACHO counterpart. The ISO-MCMS name is given in Col. 1, the distance in arcsec to the first possible MACHO counterpart is given in Col. 2 and in some cases the reason for the missing cross-identification is written in Col. 3. Too few data points means that there are not enough points to characterise the shape of the light-curve. This would be useful to recognize a MACHO counterpart within the ISO astrometric precision.
Table 4 provides the magnitudes from the different databases, the bolometric magnitude (see next section) and the parameters that describe the dominant pulsation of all the sources in the sample with an extracted light-curve (458). This table is also available electronically at the CDS and the first 10 lines are given as an example (Table 4). The content of the table is the following: ISO-MCMS name (Col. 1), IJKS DCMC magnitudes (Cols. 2-4), JHKS 2MASS magnitudes (Cols. 5-7), LW2 and LW10 ISO magnitudes (Cols. 8 and 9), the apparent de-reddened bolometric magnitude (Col. 10), period, amplitude, flag and quality parameter derived for the light-curve in the MACHO-red bandwidth (Cols. 11-14) and in the MACHO-blue bandwidth (Cols. 15-18).
Values of 99.99 for the magnitudes and of -99 for period and
amplitude indicate missing data. Delmotte et al. (2002)
have shown that
but we did not apply this
correction to Table 4.
Amplitudes (A) are the difference between
the minimum and the maximum value of the MACHO intensity and are
expressed in
In a handful of sources this
calculation might be biased by spurious data points with a
magnitude excursion compared to the sinusoidal behaviour of the
light-curve. Maybe these are real points and represent a
flare. The period is in days.
|Figure 1: Location of the fields observed by ISO (continuous line) and MACHO (dashed line) in the SMC. The ISO fields lie in the bar of the galaxy and are each in size. Both right ascension (RA) and declination (DEC) are in degrees.
|Figure 2: Histogram of the absolute distance between the 2MASS counterpart of an ISO-MCMS source and the corresponding MACHO source.
With the availability of magnitudes from the I band to the mid-IR band LW10, it is possible to determine quite precisely the bolometric magnitude of the sources in the sample by integrating under the spectral energy distribution (SED). This integration has been done by fitting a spline to the SED profile in the plane , extrapolating linearly to zero flux at zero frequency, and also extrapolating linearly at the other extreme of the SED through the two near most points. The SED of all the sources detected by DENIS and ISO were inspected one-by-one to exclude those that are either too red or too blue to describe satisfactorily their SED with the available measurements.
The adopted extrapolations represent the SED very well, almost independently of the circumstellar opacity for all M spectral subtypes (Loup et al. in preparation). That article gives a detailed determination of the multi-band bolometric correction for AGB stars by combining data from the major survey instruments: DENIS, 2MASS, ESO, IRAS, ISOCAM and MSX. The bolometric correction is obtained from the different combination of pass-bands and a theoretical model for the SED. This is compared to the correction obtained from the integration under the SED using a spline or a linear fit through the flux points. A fairly well sampled SED that detects most of the energy emitted by the objects in a set of characteristic bands is a necessary condition to derive a good bolometric luminosity ( ) for stars of different M spectral subclass and C stars.
The best wavelength coverage for the data in the sample studied here is obtained by combining DENIS and ISO magnitudes. Though 2MASS KS magnitudes exist for 455 sources, DCMC-JKS magnitudes exist for 366 sources and DCMC-IJ mag exist for about 450 sources. On the one hand it would seem natural to combine IJ DENIS magnitudes with 2MASS-KS magnitudes and the ISO magnitudes, for the same sources, to derive the bolometric magnitude. On the other hand the DCMC-IJKS magnitudes were obtained by simultaneous observations and this is a unique constraint for the SED profile.
Note that the amplitude of variation in the mid-IR bands can be as high as 1 mag (e.g. van Loon et al. 1998; van Loon et al. 2001), this effect may influence the shape of the SED during the variability cycle. The constraint of the I band to the shape of the SED at higher frequencies is very important for optically thin AGB stars because the peak of the SED is at about KS. In Loup et al. (in preparation); we show that the linear extrapolation to zero flux at the longer frequencies starting from the flux in the Jband subtends a larger area than the extrapolation starting from the flux in the I band. This effect overestimates the bolometric magnitude.
Prior to the calculation of the flux emission in the different bands and the integration under the SED we de-reddened the data adopting the extiction law by Glass (1999). For the DENIS pass-bands we used [AV:AI:AJ:AKS=1:0.592:0.256:0.089], and we assumed zero absorption in the ISO wave bands. We used RV=3.1 and E(B-V)=0.065, the latter is the average of the measurements, in the SMC, discussed in Westerlund (1997). The zero-point of the bolometric scale is computed with: and erg cm-2 s-1. A comparison of our bolometric magnitudes with the relations obtained by Alvarez et al. (2000) and Montegriffo et al. (1998) is given in Appendix B.
There are a few differences that depend on the way the two samples were selected and the light-curves extracted: in the SMC there are sources with longer periods because the MACHO data cover a longer time range than the EROS2 data. Thus it is possible to identify longer periodicities. Also there is a relative lack of SMC sources around the tip of the red giant branch (TRGB) because the LMC sources were selected from the DCMC and not among those sources detected at 7 and 12 m. It may be that AGB stars that are not yet in the TP-AGB phase or are in a very early phase of their TP-AGB evolution have a mid-IR emission below the ISO detection limit. The ISO survey was indeed designed to find mass-loss, not to detect sources without circumstellar extiction.
The analysis of the light-curves of LMC sources detected by ISO has just started. The KS magnitudes are always a one-epoch measurement, and coupled with the amplitude of variation, that in the KS band can be as high as 1.5 mag for OH/IR stars, prevent us from detecting a difference (if any) in the width of the PLRs due to metallicity. The same situation holds for stars in the Bulge (Alard et al. 2001), which have the additional disadvantage that the distance to the AGB stars is too uncertain to find all four PLRs. Furthermore, AGB stars in stellar clusters are too few to outline the presence of one and possibly two PLRs. There is evidence that in the elliptical galaxy NGC 5128 one and maybe two PLRs exits for LPVs (Rejkuba 2002).
The atmosphere of AGB stars is dominated by molecules of TiO and VO if the star is O-rich ( ) or by molecules of CN, C2 and other carbonaceous molecules if the star is C-rich ( ). Stars of both types are easily statistically distinguished in the (J-KS, KS) colour-magnitude diagram (Fig. 4a) because of the different strength of the molecular absorption bands at these particular wavelengths (Cioni et al. 2001; Loup et al. 2002). The dividing line at (J-Ks)=1.33 takes into account the shifts calculated by Delmotte et al. (2002) between 2MASS and DCMC magnitudes and has been defined in Cioni & Habing (2003) for the whole AGB population of the SMC. It was also formerly checked by Cioni et al. (2000) via the cross-identification with the large sample of spectroscopically identified C-rich stars of Rebeirot et al. (1983). Filled symbols in Fig. 3 indicate C-rich objects. In Fig. 3b they define relation B and C, and dominate relation D (possibly offset from the oxygen-rich stars).
In the LMC (Cioni et al. 2001) C-rich stars occupy only the brightest part of the PLRs, thus in a lower metallicity environment, such as that of the SMC, C-rich stars form at lower masses, unless these stars are in the luminosity dip that follows a thermal pulse or at the minimum of their light-curve. Menzies et al. (2002) recently showed that the top magnitude of the AGB stars in KS in the dwarf galaxy Leo I ( ) are mostly carbon stars. They have J-KS>1.1. The value of the J-KS that discriminates between O-rich and C-rich stars is a function of metallicity. The lower the metallicity, the bluer the colour. Obscured AGB star candidates (J-KS>2) might also be of C type (50% level) and the observation at two different epochs indicates that at least one of these object might be a Mira variable ( ).
The scatter in the PLR of the sources in this study results from the unavailability of bolometric light-curves. However, it is consistent with the sigma associated with the relation derived by Feast et al. (1989). Estimating the magnitude of this effect would be valuable for studies that plan to use AGB stars as tracers of the star formation history of systems as far as 250 kpc (Kucinskas et al. 2002). This preliminary investigation on the use of AGB stars concerns mainly early-type AGB stars which vary with amplitudes much below that of Mira-type stars. On the other hand, Kucinskas et al. combined broad-band observations from the literature. It should not be neglected that the amplitude of variability of AGB stars is different in each photometric band. Only simultaneous observations in different bands, such as those that will be available with GAIA, provide a coherent SED from which a single-epoch bolometric magnitude can be derived.
Finally we conclude that a large amplitude and a large value
of q indicate a clear and regular light-curve; thus a Mira star.
There are some sources of large amplitude and with
a large value of the quality parameter suspected of multi-periodicity.
Their main period does not correspond to relation C.
A few Mira variables in sequence D
have been found by Alard et al. (2001). On the contrary, this
PLR could be populated by binary stars with an AGB companion (Wood et
al. 1999). In what follows we mainly discuss the properties of the
stars with a light-curve in the red band of MACHO
and f=1 or f=6.
|Figure 3: Diagrams for the sources in the sample with a MACHO-RED light-curve and f=1 or f=6. a) KS versus relation. Letters ABCD identify the parallel sequences as defined in Wood et al. (1999). Filled symbols indicate probable C-rich objects. b) PLRs and overplotted theoretical tracks by Vassiliadis & Wood (1993). The numbers indicate the initial mass of the stars in each track. c) Amplitude distribution as a function of bolometric magnitude. d) PLRs for sources with an amplitude above the dashed line indicated in c), q>100 and f=1. The continuous line is the Mira PLR fitted through the crosses corresponding to P<420 days obtained by Feast et al. (1989); a distance modulus of m-M=18.99 (Cioni et al. 2000) has been applied. Symbols identify O-rich stars (open circles), C-rich stars (filled circles) and Feast et al. (1989) variables (crosses).
Mira variables lie on one PLR (Feast et al. 1989) and SR occupy this and other PLRs according to their mode of pulsation (Wood et al. 1999; Cioni et al. 2001; Noda et al. 2002; Lebzelter et al. 2002). If Mira variables are selected as discussed in Sect. 4.3 then they are clearly concentrated on the C PLR. This selection criterium is based on the amplitude of variation. However, the sources are the most regular as well (q>100).
Whitelock et al. (1997), by analysing the light-curves of a dozen C-rich AGB stars in the Milky Way Galaxy, showed that the distinction between Mira and SR variables is not necessarily very clear among carbon stars, and may not be useful as a distinction for C-rich stars as it is for O-rich stars. Figure 4b shows the histogram of the distribution of the amplitude of variation separately for O-rich and C-rich stars. Perhaps there is a distinction between Mira, the pulsators at the tail of the amplitude distribution(s), and SR. Both O-rich and C-rich sources have a histogram with a dominant peak at about and , respectively, and a tail to larger amplitudes. The fact that C-rich stars have on average larger amplitudes than O-rich stars is different from what was found in the LMC. There, both histograms had the same distribution (Fig. 4 in Cioni et al. 2001). The same histogram but for the amplitudes derived from the BLUE light-curve shows that O-rich stars peak at about A*100=50 and C-rich stars at about A*100=100. This confirms that the average amplitude is larger in the blue than in the red spectral domain.
Figure 4 in Cioni et al. (2001) shows that O-rich AGB stars in the LMC have a strong broad peak between and 2.0, and a lower peak at about , while C-rich AGB stars are homogeneously distributed from to 2.5. The first LMC peak of O-rich AGBs is probably a consequence of the selection criterium used to define the two samples. The SMC sample is extracted from sources with an emission in the mid-IR, these stars are brighter and with longer periods than the stars in the LMC sample which were selected from the DCMC database. The difference in strength is probably due to the mean difference in the AGB type between the two Clouds. There are more carbon stars in the SMC which is on average more metal poor than the LMC (Cioni & Habing 2003). This effect is also important for the sources populating relation C which are predominantly C-rich in the SMC and associated to the peak at about . That the majority of accepted Miras in the SMC are carbon stars was first recognized by Lloyd Evans et al. (1988) as the result of a search for large-amplitude red variables in the Radcliffe Variable Star Field. The longer time range spanned by the MACHO observations allows to detect periodicities above which was about the limit reached in the LMC study using EROS light-curves. The large number of sources detected in the SMC at these periods are likely to be multi-periodic. Their secondary period will be part of relation A, B or C, thus they will enhance the number of O-rich stars between and 2.5. In more detail we found that in our sample, among those with a red light-curve and q>15, 24 sources have . These sources have which, taking into account the differences between the various period determinations and the mean, gives a period ratio from 1.5 to 2.
The same sample of LMC stars analysed by Cioni et al. (2001) was afterwards studied by Lebzelter et al. (2002) using the AGAPEROS datasets. Ninety per cent of their sources were classified into: regular, SR, irregular and other variability classes. Their analysis covers a time window of up to 900 days and is thus incomplete for the longest periods, but it is more complete for sources with an amplitude of variation below 0.1 mag. The authors found that the period distribution of regular variables has two peaks: one at and the other at . The latter is probably formed by Mira stars. SR variables peak at about . The peak at the shortest periods is probably the same as the one found here. The peak of mostly Mira stars corresponds to the location of the peak of the C-rich SMC stars. In the Baade's window, Glass & Schultheis (2002) found that most of the late-type M giants have ; those few with a secondary longer period have about . The histogram that can be derived from their Fig. 2 is very similar to that of O-rich stars in the SMC (Fig. 4c).
In a similar fashion to the LMC sample (Fig. 7 in Cioni et al. 2001), variable stars of a different type and variability class are plotted in the colour-magnitude diagrams (CMDs) in Fig. 5. The distinction has been made as follows: Miras have independently of their type, and a regular light-curve with a well defined single periodicity. Similar sources but with a smaller amplitude of variation are SRa stars. SRbs are those stars which indicate the presence of a secondary period. Note that in this last category there is no distinction based on the amplitude of variation. As in the LMC, Mira stars are uniformly distributed in the regions where optically thin O-rich and C-rich, and also more optically thick stars, are located (Fig. 5a). SRa and SRb are almost equally distributed within the two branches of O-rich and C-rich optically thin AGB stars. Figure 5d shows the distribution of the sources that could not be classified in one of the three categories either because the light-curve has a too low S/N or it is extremely irregular. Most of these stars (180 out of 194) have A>10, thus they are variable stars and lie above the TRGB, KS=12.62 (Cioni et al. 2000). It is possible that stars considerably brighter than KS=10 are supergiants and that fainter stars at about (J-KS)=0.4 are foreground objects. Schultheis et al. (2000) found variable star candidates at (J-KS)<1. They conclude that it is probably a result of uncertainties in the determination of extinction. However, they find a displacement of the Bulge stars detected as variables in both J and KS to bluer colours than the sequence indicated by all detected ISO stars in the diagram (LW2-LW3, LW3). It would be interesting to know if some of these stars are supergiants and of which type.
Finally we conclude that all the sources in the sample are variable
stars because they have amplitudes above or equal to 0.1 mag either
in the RED or BLUE wave band. A similar conclusion was reached by
Alard et al. (2001) for a sample of sources in Baade's window
detected at 7 and 15 m. The emission at the longest
wavelength is a signature of
mass-loss rate. Using their dependence between
and the
mass-loss rate and assuming that the mass-loss rate of highly
evolved AGB stars does not depend very strongly on metallicity
(van Loon 2000), we derive that
the sources in the present sample lose mass at a rate
), but most of the objects have
which corresponds to a mass-loss rate of about
Note that a complete study of the dependence of mass-loss
includes temperature, mass and outflow velocity as well.
|Figure 4: Variable O- and C-rich AGB stars a). The histogram of the amplitude of variation b) and that of the period distribution c) are shown for sources of both types. The amplitude as a function of period is shown in d).
The m LW2 filter does not include a large dust contribution for non-Mira sources and it is mostly a measure of the photospheric emission. On the other hand, for stars with a relatively thick circumstellar dust envelope, this band is strongly affected by the presence of dust (Alard et al. 2001; Omont et al. 1999). The m LW10filter, which is very similar to the IRAS m band, includes the m silicate and the m SiC dust features. Thus the colour (K-LW10) provides a strong indication of the amount of circumstellar dust for the entire sample.
Figure 6 shows the colour magnitude diagram (KS-LW10, LW10) for the sources in the present sample, distinguishing between Mira and SR variables. Except for a few SR all the sources with (KS-LW10)>2 are Mira variables (Fig. 6a). From the location of some K- and M-type supergiant (SG) stars in the ISO-MCMS one derives that they have (KS-LW10)<1 and LW10=8. They follow a sequence that extends almost vertically to fainter magnitudes, but the nature of those sources with LW10>10 is not confirmed. Bright O-rich LPVs would have (KS-LW10)=3 and LW10=7. These stars would have a late M subtype and not many of them are expected in the SMC. A quantitative statement will be possible once the study of the LMC LPVs detected by ISO is completed. A few SRb stars populate the fainter part (Figs. 6b,c). There are many supergiant stars along the whole sequence that were not classified in any of the three categories (Fig. 6d). It is thus not surprising that their light-curve is more difficult to classify because of a low S/N and irregularities. Thus, except for a few stars overlapping the region occupied by SR and Mira stars we are able to distinguish sources with a poor or non-regular light curve. A more careful look at the near-IR colour-magnitude diagram (Fig. 5) confirms that the unclassified stars with (J-KS)=1 or a bluer colour are experiencing the supergiant phase because AGB stars have overall (J-KS)>1. This is quite a good criterion to discriminate between supergiant and AGB stars, though the distinction is better achieved in the combined near- and mid- infrared diagram (Fig. 6).
Most carbon stars are located at about (KS-LW10)=1 and 8<LW10<11(Fig. 6 - filled points); the sequence of dust obscured C-type stars extends to redder colours but the LW10 mag follows a shallower slope such as (KS-LW10)=4 at LW10=8. On average C-rich stars are redder than O-rich stars.
Planetary nebulae and emission line objects, included in the ISO-MCMS catalogue, also have red colours ( KS-LW10>2) but they have fainter magnitudes with respect to Mira stars and are roughly located in a parallel sequence. Three of these objects are present in Fig. 6d. The object at LW10<8.5 and KS-LW10>4 is a known carbon star while the object with the same LW10 magnitude and a bluer colour is a known variable M giant, because of its red colour we erroneously classified it as a carbon star.
Figure 7 shows the colour-colour diagram of the variables identified in this study. The O-rich sources with (LW2-LW10)>0.4 are AGB stars or red supergiants. These AGB stars have a significant circumstellar extinction. This is also the colour of obscured O-rich and C-rich stars, and those with the highest amplitude of variability have (KS-LW2)>1.5. O-rich stars without a considerable mass loss have approximately (LW2-LW10)=0 but can have 0<(KS-LW2)<1. There is not a remarkable distinction between SRa and SRb pulsators. At about (KS-LW2)>3.5 one can find PN and emission line objects.
It seems (Fig. 7d) that we may have missed the classification of a few Mira variables, O-rich and C-rich SR stars. At this stage it is worth going back to the specific light-curves to find out the reason of this missed classification and to perhaps identify some peculiar objects. Among the objects with KS-LW2>1.5 (Fig. 7d) J005113.6-731035, a known carbon star (RAW 658), has a flat light-curve, while the light-curve of J005136.5-732016, identified as a PN, is irregular. Another PN is J005157.9-731421 which may have a regular light-curve with an amplitude of about 0.8 mag. The periodogram of the other objects, J004849.4-731627 (emission line star), J005212.9-730852 (variable M giant) J005304.7-730409 and J010020.6-730648 (BMB-W 29 carbon star) shows a very low amplitude with flare-like events.
|Figure 5: Colour-magnitude diagrams (J-KS, KS) for variable stars classified as Mira a), SRa b) and SRb c) according to their periodicity and amplitude of variation. d) is the same diagram for variable sources which could not be classified in one of the three categories because of low S/N or an extremely irregular light-curve. The vertical dotted line indicates the separation between O-rich and C-rich stars as in Fig. 3.
Most of the DENIS sources in the present sample were observed in December 1996 while 2MASS observations date August 1998. This difference in time of about two years may allow us to recognize variable stars by comparing their detection in the near-IR bands of DENIS and 2MASS. Figure 8 shows the distribution of these differences for all the sources in the sample. We checked that the separate histogram of sources with an assigned MACHO periodicity is the same as that of sources with (a period was not assigned but the source is probably a variable). The histogram does not account for the systematic difference between the 2MASS and DCMC magnitudes as measured by Delmotte et al. (2002). Selecting only the variable stars with the largest amplitude produces a similar histogram. The displacement from zero indicates that the sources are variable stars. Note that the difference is approximately the same in the J and KS bands.
The most obscured stars have large (KS-LW2) and (LW2-LW10)
colours. This indicates sources with a thicker circumstellar envelope
and allows to easily distinguish AGB stars from supergiant stars and
other classes of objects such as PN and emission line sources. The
difference between the 2MASS and DCMC magnitudes suggests that most of
the sources in the sample are variables.
|Figure 6: Colour-magnitude diagrams (KS-LW10, LW10) for the same groups of sources as in Fig. 5.
|Figure 7: Colour-colour diagrams (KS-LW2, LW2-LW10) for the same groups of sources as in Fig. 5.
|Figure 8: Histogram of the differences between the 2MASS and DCMC magnitudes of all the sources in the sample.
The first author is very grateful to J.-P. Beaulieu for providing the algorithm to detect the periodicities. This paper utilises public domain data obtained by the MACHO Project, jointly funded by the US Department of Energy through the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48, by the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616, and by the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the Mational Science Foundation.
In order to improve our understanding of the identification of Mira-type variables we decided to re-analyse the LPVs studied by Feast et al. (1989). These are the Mira stars that define the period-luminosity relation in the LMC. We could find the B1950 coordinates of 42 out of the 55 sources with a "good'' or "fair'' light-curve as classified by Feast et al. (1989). We could not find in the literature the coordinates of the objects from the sample of Glass & Lloyd Evans (1981) and for three objects from the list of Glass & Reid (1985) or Reid et al. (1988). However, there still remain enough sources for our purpose.
We searched in the MACHO database for the light-curve of the closest LPV to these 42 sources. The identification was easy in most of the cases because of the highly regular and large amplitude light-curve typical of a Mira star. Five sources (W158, GR28, GR4, RGC91, RGC89) are unfortunately outside the fields observed by MACHO. For one source the MACHO web site gives a persistent initialization error (W94) and for four additional sources (GR13, GR21, RGC37, RGC53) we could not find a nearby counterpart (a first possible candidate is further than 8 ). Only one source (W30) has two possible MACHO counterparts and due to the low accuracy of the initial coordinates compared to the MACHO coordinates we decided to remove this source from the discussion. Finally we could successfully extract the light-curves of 31 sources.
We determined the main periodicity, as described in Sect. 3, of the sources with a MACHO-red light-curve. We obtained periods that are at most 20 days different from those derived by Feast et al. (1989) except for 4 sources which result to have a period coincident with one of the extremes of the searching window (GR2, GR3, GR18 and GR29, they have been removed from the following analysis) and source GR17 for which we derive a period of 51 days shorter. The period of source RGC20 falls in the region of aliases (Sect. 3), thus the source has been removed from the following discussion. The quality parameter of the 26 sources with a convincing period determination is always above 100 and the difference between the assigned period and the mean of all the determinations with q>15 is of the order of 1 day for most of the sources but always below 10 days. These numbers may be different in the case of MACHO-blue light-curves.
Table A.1 lists the name of the sources (Col. 1), the coordinates at the epoch J2000 precessed from the original coordinates (Cols. 2 and 3), the MACHO identification code (Cols. 4-6), the distance in arcsec between the Feast et al. (1989) source and the MACHO counterpart (Col. 7), the period, amplitude and the value of the quality parameter for the red light-curve (Cols. 8-10).
We conclude that by selecting, from our sample, large amplitude
sources with a single periodicity and q>100 we are identifying Mira variables
of the same type as those studied by Feast et al. (1989). They define
a tight PLR and the small scatter in Fig. 3d is probably due
to the availability of only one epoch bolometric magnitude. Note that with
this selection criterion we also find sources at very bright magnitudes
which deviate from the extrapolation of the PLR defined only
for sources with P<420 days. We estimate from Fig. 3b that these
stars have
and as previously noted by Feast et al.
(1989) the PLR breaks at high masses. These stars are likely to be
"over-luminous'' as a result of Hot Bottom Burning (Zijlstra et al.
1996; Whitelock et al. 2003). However, because of their very
high luminosity they could also be supergiants.
|Figure B.1: The bolometric correction BCI as a function of the I-J colour for the O-rich (open circles) and C-rich (filled circles) variable stars in the sample. The continuous line is the relation derived by Alvarez et al. (2000) for cool O-rich stars.
|Figure B.2: The bolometric correction BCK as a function of the J-KS colour for the O-rich (empty circles) and C-rich (filled circles) variable stars in the sample. The lines are the relations derived by Montegriffo et al. (1998) for Population II giants of low (dashed line) and high metallicity (continuous line).
Figure B.2 compares the bolometric correction obtained as in Sect. 3.1 with the relation derived by Montegriffo et al. (1998) for Population II giants of low ( ) and "high'' metallicity ( ). They used . Their relation was defined up to (J-K)=0.8 but being the metal-poor relation very close to the metal-rich relation at redder colours we consider the latter as a possible extrapolation. This results in a fairly good fit for the O-rich variables while C-rich variables lie systematically below the relation. This is a similar effect as that observed for BCI versus I-J (Fig. B.1). The giants in the sample of Montegriffo et al. (1998) are members of galactic globular clusters. C-rich stars are rare members of these systems. The spectral range covered by the observations is limited to m (L band) and they derive the bolometric magnitude by integrating the SED which is previously re-constructed by means of a set of Plank functions at a given wavelength. These effects may influence the correction to be applied to the flux measured only in the K band. Besides the m filters used in both studies are not strictly the same. We conclude that we cannot at present compare the correction for C-rich stars while O-rich stars are qualitatively in agreement. It would be useful to compare stars of other galaxies in the Local Group at a different metallicity.


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About Borahm Lee
Borahm Lee tickets are on sale now and they are going fast. Be there for a stop on the 2020 Borahm Lee concert tour and get ready for an unforgettable night. Browse concert tickets for Borahm Lee and get ready for the show of a lifetime!


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Part-time Student Data Premium Project Assistant (H/F)
Fecha de inicio
Tipo de contrato
Contrato prácticas jornada parcial
Jornada laboral
Full time
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You are a student in a business, engineering or computer science school, you want to invest in project for ARaymond in terms of research and management of internal and external product data, and you have an IT background.
You want to work in an internationally oriented company and you speak English fluently.
You are rigorous and organized and you are not afraid of Excel.
Duration : 12 months
Start : 01.09.2020


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In case you missed it: Learn how to navigate open enrollment and help your employees make informed decisions this fall ..
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Date : Friday, January 18, 2019
Ensuring higher profits in 2019 means taking a hard look both at where you can grow and where you can operate more efficiently. An investment in payroll and Human Capital Management (HCM) software can be a good place to start. ..


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Snow Teeth Whitening Review: How Does It Work? How To Completely Whiten Teeth Naturally
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Kevin Brooks
Chief, Total Force Human Resource Management (HRM)
U.S. Air Force
Mr. Kevin W. Brooks is Chief, Total Force Human Resource Management (HRM) Policy and Publications Analysis Division and Senior Policy Advisor, Headquarters Air Force, the Pentagon, Washington, D.C. He is tasked to develop and maintain Total Force A1 policies to enable the enterprise strategic plan, vision, and concept of operations (CONOPS); define and build a total force integrated HRM community; and facilitate integration of HRM policies. He plans, organizes, and directs the activities of Deputy Chief of Staff for Manpower, Personnel and Services, Publications Cell, to comply with legal and regulatory requirements and meets customer needs. Develops, interprets, and implements policies and procedures needed for the effective implementation of DoD policy guidance to the Total Force HRM Enterprise, in conjunction with overseeing and monitoring a quadrennial policy review cycle to keep all 34-, 36- and 38-series publications current. Prior to his current assignment, he was an Air Staff Division Chief and 38F Career Field Manager.
Mr. Brooks has had a diverse Air Force career working within manpower, personnel, and services. He commanded a mission support squadron, a force support squadron, served as a deployed J-1 and a congressional liaison officer. His headquarters staff tours include multiple tours at HQ USAF, HQ JFC Brunssum (NATO) and HQ AFOSI.


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"Elixir's last forever, and they only get better with a little age on them. They rarely go out of tune - outdoor festivals, indoor venues, wherever - our sets aren't interrupted by extended tuning montages anymore!"- Cameron Briley, Bassist, @The_Skeleton_Krew . photo: Lisa Adkins . #elixir #elixirstrings #elixirartist #bassplayer #strings #guitarstrings #geartalk
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The Back Porch Podcast - Ep. 48: The Skeleton Krew "Graveyard Manner"
August 28, 2018
The Back Porch is back after a short month off with Hunter Cross and Cameron Briley of The Skeleton Krew. They are a busy troupe and kindly take some time out to talk with us and play a few songs without the consent of Cameron's agent. Oops! We learn Hunter tricked Cameron into to being in the band,"organically", we take a vague trip to the twilight zone and Steve learns they speak Portuguese in Brazil. Yet, another fun filled episode to either strengthen what you already know about this group or introduce you to something new. Enjoy!
Tennessee's Strangest Duo
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I see, thanks.
Excellent -- but how do I contact the support team?
"Cannot get the list of trackers"
dpdpdp posted a topic in Sync TroubleshootingSince updating to version 2.6.0, the two machines that I keep in sync both display the error message "Cannot get the list of trackers". I have checked everything listed at https://help.resilio.com/hc/en-us/articles/210587126-Cannot-connect-to-trackers. All the relevant ports seem to be open, and I can download the tracker address file in my browser. In any case, one of the machines is in my home, behind my router, and the other is at my university office, so the problem can't be localized to one router or location. I did not have this message before the update. Help?
".!sync" files
dpdpdp posted a topic in Sync TroubleshootingOn one of my synced machines, the hidden ".sync" folder contains many files with the extension ".!sync". The other synced machine does not. Is this how it should be, or is this situation telling me something (for example, about why I have continued intermittent syncing problems)?
any information? (going through this yet again)
About a year ago, my formerly rock-solid installation of Resilio Sync on my laptop and office desktop Mac became unreliable. I would suddenly realize that nothing had been syncing for a while, and when I checked it would appear that sync of one or more folders was stuck at some percentage. Often when this happens it is also impossible to quit Resilio Sync without force-quitting it. Resilio support had me send log files and replied that contrary to the evidence of my eyes, there was no problem — so I abandoned that interaction. Eventually I discovered that quitting Sync and deleting the folder ~/Library/Caches/com.resilio.Sync reliably solves the problem. But it would be great if the underlying issue could be fixed. What can go wrong such that deleting the cache folder solves the problem, and how can that be prevented?
Resilio Sync and MacOS High Sierra public beta?
dpdpdp posted a topic in Sync General DiscussionIs any information available about whether Sync will work if I update to the current public beta of MacOs 10.13 High Sierra? (I understand it's a beta, your mileage may vary, etc. Just not seeing any reports on the sites that list compatible vs. incompatible apps.) Many thanks.


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Kenneth A. Schwab (Ken) is a lifelong resident of Missouri. He attended Missouri State University in Springfield, MO and in 1978 graduated with a Bachelor of Science degree in Economics. After a brief employment with Great Southern Bank and National Cash Register (NCR), Ken became the General Manager of Wilhoit Properties, Inc. in 1981. Since this time, Ken has implemented numerous property management policies and procedures in the supervision of residential and commercial property management. In 1984, Ken obtained his Missouri State Real Estate License and has since directed his efforts toward the sale and leasing of over $300,000,000.00 in commercial and investment property in Southwest Missouri. Ken is also an investor in several investment properties including residential apartment buildings, commercial retail centers, commercial office buildings, and development land. Married to Teresa Schwab in 1979, they have 2 adult children, Ashley Quinn and Branden Schwab both of Springfield.
Missouri Licensed Real Estate Salesperson - 1984
Professional Associations:
Greater Springfield Board of REALTORS® -Former Board Member
The Missouri Association REALTORS®
The National Association of REALTORS®
Springfield Business Journal Economic Impact Award Winner for Commercial Real Estate Category
Community Involvement:
Oakstar Bank - Past Board Member
Land Clearance for Redevelopment Authority - Past Board Chairman
Springfield Public Building Corporation - Past Vice-President
Springfield Catholic Schools Development Board - Past PresidentSpringfield Southeast Rotary - Past Board Member/ Current Member
Red Cross - Greater Ozarks Chapter - Past President
Dogwood Council - Girl Scouts, USA - Past Board Member
Holy Trinity Catholic Church - Member
Contact Details:
417-860-1502 (mobile)
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I'm a big Groovy enthusiast, but I only use it myself for build/deploy scripts.
A real pro demonstrated Groovy's power last night:
Paul Woods ran us through 90 minutes of groovy features last night, and demonstrated how powerful the language can be in the hands of someone who works with it exclusively every day for a year. Read more »


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Trials of Osiris resurrected for Destiny 2 up coming month
Bungie will resurrect Trials of Osiris, Destiny's toughest PVP mode, within just Destiny 2 on 13th March.This revamped edition of Trials appears to be set to attribute lots of what created the primary fantastic: three-on-a few groups, electric power-enabled gameplay, as well as the return of basic D1 maps these kinds of as
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Spider-Gentleman artist discusses pickle of picking Peter Parker's pecs
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"Cosy management sport about dying" Spiritfarer gets initially gameplay trailer
Coming to Computer and consoles later this year.Thunder Lotus Games, the Montreal studio guiding Jotun and Sundered, has released the first proper gameplay trailer for Spiritfarer, its forthcoming "cosy administration video game about dying".Spiritfarer casts players as Stellar, a ferrymaster to the deceased, charged with roaming the seas and fulfilling the last requests of
Shock! RimWorld launches Royalty DLC
Here is a little something to brighten up a reigny Monday early morning: RimWorld's free of charge 1.1 update is rolling out to absolutely everyone right now, and far better however, a surprise DLC referred to as Royalty has launched. Never be concerned, it really is not a fight royale. The growth suggests
CD Projekt Red is now the second-greatest online video game company in Europe
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It is the most fantastic time of yr: February! It can be also still Xmas, according to Anthem, for the reason that the video game however has its decorations up - even now, a total two weeks right after the original tweet, which pointed out that open up invitation for terrible luck, went
Activision goes to war over Get in touch with of Obligation: Modern Warfare fight royale leaks
Activision is fighting Call of Duty: Modern Warfare struggle royale leaks with subpoenas and on line takedowns.Present day Warfare's impending fight royale, reportedly dubbed Warzone, is a single of the worst-kept secrets in all of online video games. When it stays unannounced, players have observed them selves unintentionally transported into its tutorial, and
Trendy change-based tactical horror RPG Othercide demonstrates off its monsters in new trailer
Coming to Pc this summer.Target Household Interactive has unveiled a new cinematic trailer for Othercide, developer Lightbulb Crew's wonderfully moody change-primarily based tactical horror RPG.Othercide was initially unveiled early final 12 months, and it is an immediately arresting proposition - sporting a stark monochromatic aesthetic minimize as a result of with offended streaks of
Crytek and Cloud Imperium Games settle Star Citizen lawsuit
Joint stipulation of dismissal to be filed within 30 days.Star Citizen developer Cloud Imperium Games has settled its lawsuit with Crytek over the alleged misuse of the latter's CryEngine.Crytek's lawsuit, which first came to light last December, argued its licence with Cloud Imperium only granted the Star Citizen developer the right to use CryEngine