The following are movies or feature-length home videos featuring Al in one way or another!
Al was red hot in 1984 coming off the success of "Eat It" and the In 3-D album. That's when Twenieth Century Fox asked him to write and record the main-title song for their upcoming gangster spoof, Johnny Dangerously. Directed by Amy Heckerling (Fast Times at Ridgemont High), the movie follows the sudden rise of a Chicago crimelord (played by Michael Keaton) who is at odds with his district-attorney brother (Griffin Dunne).
The theme song that Al came up with, the cool original "This Is The Life," perhaps better captured the spirit of the 1930s than the movie actually did. The song was not only used in the movie, but it also became a single and a music video. However, when the movie was released on home video, the song was nowhere to be found due to some still-unclear legal-clearance snafu (yet it was in the movie during most television broadcasts). It wasn't until the 2002 DVD release that the song was restored to the opening credits. Almost as a sort of retro-vindication, the DVD also includes the movie's original trailer, which proudly proclaims, "Theme song by 'Weird Al' Yankovic."
Unfortunately, in a situation not unlike that of 1996's Spy Hard, once Al's song ends, the movie sputters. It starts off with a great sight gag, but then quickly slows down to a comic pace and style somewhere between Police Academy and Mel Brooks's lesser comedies. Although this spoof is hardly as bad as Scary Movie 2, everyone involved has since done better work.
The very first Weird Al home video release, doubling as a semi-fictitious biopic and as a compilation of the music videos made up to that point. It can seem a little bogged down at times, but overall it's very funny and amazingly well done for a direct-to-video production (consider this is 1985, when a direct-to-video movie was almost unheard of!).
The Compleat Al is also known for featuring a handful of clips from the first two Al-TV specials, an exclusive mini-video for "Midnight Star" (depicting Al's tour crew fixing up his hotel room), and a lot of Nick Yankovic's home movie footage of young Al growing up (mostly spinning around and falling).
A squashed version of The Compleat Al aired on Showtime in August 1985. Although there has been some occasional "official" word of otherwise, the video itself has been out of print for a little over a decade. It's actually pretty hard to find, even in video rental stores. Maybe one day in the future it will be released on DVD...yeah, like that'll happen!
How do you make a bizarre animated movie even more bizarre? Give it a hip, new age soundtrack!
Scotti Bros. released the soundtrack album over the summer of 1986, and the resourceful record label included their headlining comedic musician Weird Al. Instead of Al creating a new song for the movie as he did in 1984 for Johnny Dangerously, Scotti Bros. simply took the title track from Al's previous album, Dare To Be Stupid. The song was used effectively in the movie as the "theme" for the planet of the Junkbots.
And let's not even go into the fact that one of the new songs in the movie, "The Touch" by Stan Bush, is the same song Dirk Diggler records in Boogie Nights!
The Transformers: The Movie didn't do great at the box office, but it became an immediate cult hit. For the longest time the video was out of print in the United States, while at the same time various "director's cuts" turned up in Canada and Japan (they featured an extra line of dialogue...with a curse word! Oooooo!). Finally the king company of cult, Rhino, reissued the film on video and DVD in 2000, introducing it to a whole new generation of Transformer fans (boy, that sounded like the last line in any random Behind the Music episode!).
Produced by ex-Monkee and video pioneer Michael Nesmith and starring not-yet-critically-acclaimed director Tim Robbins and John "I will always be an aging Gen X star" Cusack, Tapeheads is about two fired security guards who try their gosh-darnedest to break into the booming video-production biz.
Despite featuring quite an eclectic mix of celebrity cameos (including the likes of Ted Nugent, Doug E. Fresh, and Don Cornelius), Tapeheads is probably only noteworthy because it contains Al's first movie appearance. And it's not even a great appearance! Al is seen shoving Cusack aside while on his way out of a building, or at least that's what it looks like. The action is so far away from the camera that it looks like the director was far-sighted (let's put it this way: if Al wasn't credited you would have thought it was a look-alike).
The original video release from Nesmith's Pacific Arts went out of print a few years ago due to Mike's financial and legal troubles with PBS, and the movie pops up on TV only once in a blue moon. So when indie and cult-movie savior Anchor Bay reissued the film on video and DVD in March 2001 (with DVD commentary by "Papa Nez," director Bill Fishman, and production designer Catherine Hardwicke), this once-rare Al oddity became readily available again.
Now this is the Al film cameo that everyone remembers! The story goes is that when Al heard that his favorite television series, the short-lived comedy Police Squad!, was going to be transformed by creators David Zucker, Jerry Zucker, and Jim Abrahams into a feature-length film in the same vein of the ZAZ team's previous Airplane! and Top Secret! (Al's favorite movie, no less!), he begged and pleaded with the producer to get him a cameo any way possible. Not that it was such a chore, since the producer was Robert K. Weiss. Weiss had previously helped write The Compleat Al--including the videos for "Like A Surgeon," "One More Minute," and "Dare To Be Stupid"--and co-directed it with Jay Levey. Weiss talked briefly about Al during the DVD commentary for the movie, saying that they invited Al back to make appearances in the other two Naked Gun films because he always remembered his lines.
For those of you who have not yet seen this comedy classic (and you must!), or did not go to a concert during which the clip was shown on the video screen, Al appears near the beginning of the film after Lt. Frank Drebin (the hilarious Leslie Nielsen) mistakes Al's airport-greeting party for his own.
The Naked Gun is a standard on cable TV, but since September 2001 the entire opening sequence (in which Frank beats up the likes of Khadafi, Yasser Arafat, and Gorbachev during a secret meeting for devising terrorist acts) is sometimes removed from broadcasts. Fortunately the movie is available on home video, because despite the recent extra-sensitive nature of terrorism it is still a gasping-for-air-hilarious scene.
For those of you who do not know, Al wrote and starred in this little-known movie called UHF about a television station and the unusually popular programming decisions made by its new manager.
To read all about it, you may want to check out our UHF Anniversary section.
MGM listened to our pleas (prompted by some web page out there) and finally released UHF as a "special edition" DVD in June 2002. The movie became a Top-10 hit in Variety and received glowing reviews after thirteen years of being called a "bomb."
This is an essential piece for any Al collection, so order the Region 1 DVD or the European Region 2 DVD now! And although the video is long out of print, used VHS copies can still be tracked down on Amazon's Marketplace.
Perhaps the most frequently asked question about Al's film work is "Where the heck is he in The Naked Gun 2 1/2?" Believe it or not, Al's cameo appearance usually kicked off the TV commercials for the movie. He's the scraggly punk who's holding the Police Squad! officers hostage at gunpoint...that is, until Frank knocks him out with the door while entering the room. Al is perhaps the only man who ever pointed a gun into O.J. Simpson's face and lived to tell about it!
The reason a lot of people can't seem to recognize Al is because it was one of his rare pre-1999 appearances in which he was clean-shaven and without glasses. Maybe a fan who had just started digging Al in only the last couple of years will be able to pick him out more easily?
And Al's official credit in the cast? "You pigs...say your prayers."--part of the Naked Gun trilogy tradition in which actors without character names are credited with their lines of dialogue.
And Al is back with the rest of the Naked Gun cast in this third outing, definitely solidifying his role in the series as a sort of running gag.
This time, however, Al is actually integral to the plot, since Frank and his wife Jane have to stop a madman (Fred Ward!) from blowing up the Academy Awards ceremony in L.A. Frank can't get in on his own since he doesn't have an invitation (nor his police badge, because he was working undercover of course). And who happens to come along? Vanna White and her date for the evening...Al! Frank and Jane not only kidnap them and steal their invitations, but they also take their clothes! Al and Vanna later show up in their underwear (Al's boxers are of course Hawaiian-styled) and finger Frank as the thief.
The movie is worth seeing just for the musical number with Pia Zadora.
As you might have just read, Al was asked to write and record a theme song for the 1984 gangster spoof Johnny Dangerously. Well, he did, and it was called "This Is The Life." The song was played over a rather generic-looking opening title sequence. However, when the film was set for a home-video release, some legal problem prevented Al's song from being included.
Twelve years later, Al is called upon once again to write an opening theme for a movie parody. Fortunately this time, Al also shot the credit sequence himself, probably to help insure that his song will be heard on the video.
Yet unfortunately for the film, Al's opening was the funniest scene in Spy Hard. The rest of the movie combined stale, repeated gags that were much funnier in the Naked Gun trilogy; gratuitous celebrity cameos by the likes of Pat Morita and Dr. Joyce Brothers; and ten straight minutes of golf jokes (yes, the writers of the film also did those nine hundred Leslie Nielsen Bad Golf videos).
But for Al completests out there, the movie also holds a special surprise at the end, an alternate version of the "Spy Hard" song. Since it's heard during the end credits, the last verse is put into the past tense. "You just saw Spy Hard!"
No, no, we're not going to give you some vague connection to this video like "Al was once inspired by a frame of 'Blood on the Dance Floor'" (LOL!) or "Al parodied every other beat in the song 'Scream' for 'Germs.'" Al actually appears in this video collection of the Gloved One's best videos...err, that apparently weren't good enough to appear on Volume I.
In Jacko's video for the song "Liberian Girl" (no, we've never heard of it, either), Mikey assembled a slew of celebrities and friends to make cameo appearances throughout. At one point, eternal dork Ricky Schroder asks, "Is that Michael?" The person he is referring to turns around, and it's Al! Later in the video, Al is seen playing his accordion to the song.
All of Al's music videos in order through 1996! It even includes the Spy Hard opening title sequence in letterbox (the actual credits were removed for legal reasons, though). Originally released only on laserdisc, the DVD edition came a year later with enhanced audio on the first six songs. If you were an Al fan and you had a DVD player, then this was a must to own (another collection has since taken that honor).
With the exception of one minor late chapter start (if you jump to "You Don't Love Me Anymore," it will go right into the song...the video's opening was accidentally tacked onto "Smells Like Nirvana's" chapter), the overall disc looks great. There are no extras outside of the cool liner notes on the packaging, but still it's a nice-albeit-modest release from Image Entertainment. Of course, this out-of-print DVD was overshadowed in 2003 by The Ultimate Video Collection, but it is still highly sought-after on the secondary market.
And for you trivia buffs out there, The Videos was also the last Al product released on the Scotti Bros. label. Soon after, Scotti's parent company All American Music was purchased by Zomba's Volcano Entertainment...and the Al legend lived on!
Feeling lucky? Then try to track down a copy of the DVD on Amazon's Marketplace. Be prepared to pay a lot.
Safety Patrol is one of those movies that you really want to like, but then you remember that Booger from Revenge of the Nerds is in it.
Depending on who you listen to, this movie had quite a unique history. Reportedly, originally it was going to be a Leslie Nielsen vehicle a la Spy Hard and was to be on television by mid-1997, but when Leslie backed down to nothing more than two fleeting "guest appearances" the entire plot was reworked to focus on young Scout Bozell (played by Bug Hall).
No matter if all that is true or not, the movie was in production for seemingly forever. Director Savage Steve Holland asked his old buddy Al to record a new song for the movie, "The Ballad Of Kent Marlow," in March 1997. The film didn't premiere on ABC until one whole year later. Unless there was some extensive Industrial Light & Magic work done to it that doesn't appear in the final cut, one must wonder what happened during that year?
Al and the band lipsynched to both the new song and "Gump" toward the end of the movie at a concert. Equally cool is that a gigantic Weird Al Macy's Thanksgiving Day Parade-style balloon was created for the film. After their scenes were shot, the band took the balloon along with them for the summer, 1997 leg of The Bad Hair Tour.
And click here to tell Disney you want it released on DVD!
Judy Tenuta stars in this smart Hollywood satire about the life of former child stars, an inspired concept that was completely tarnished in 2003 by Dickie Roberts: Former Child Star (a movie that contains a number of "coincidental" similarities to this one). Judy plays Joanie Sweeney, star of the 1960s sitcom Daddy's Little Angel, who is hoping to make her big comeback by any means necessary. Rather than getting her acting gigs, her agent instead tries coming up with bigger and more-humiliating publicity stunts for her to partake in.
This movie has two special Al connections. Most importantly is that Al makes two funny cameo appearances in the film, as do other celebrities such as Emo Philips, Burt Ward, Dana Plato, and particularly Erin Moran. Filmed in 1997, this may be the very last appearance of Al in his "classic" mustache-and-glasses guise (that is, and have the mustache be real). The other connection is that a workprint version of the movie was screened at ALCON 2000. Although the ending of this early cut was edited around for the released version to make the outcome seem more positive and less comtemplative, the end result still works while also commenting on a point made earlier in the film.
Although it's still recommended, the DVD presentation could have been a little better. Was the movie actually shot in full-frame format (that would make sense to a point, considering the film's subject), or are we being deprived of a letterbox picture? The extras only include a trailer and filmographies stolen from the IMDb. It's obvious from the end-credit sequence that outtakes exist, so where are those on the DVD? Surely a film that was in limbo for several years would warrant a commentary, right? Oh well, I guess we've been spoiled by the UHF DVD.
Al's first home-video release through Volcano Entertainment proved to be a hit, and why wouldn't it be? Al fans had been yearning for years for a live concert album. So, Al did one better and released an entire video of a performance! He even included the music videos of "The Saga Begins" and "It's All About The Pentiums" as a bonus. What a guy!
The DVD went even further by including two educational films that Al showed during Touring With Scissors, "Germs and You" and "Crimes of Carelessness." Plus there's a photo gallery, enhanced audio, and Al's commentary on the two videos. A MUCH better DVD than The Videos. It's hard not to recommend it!
Sigh......here we go. Trying to make this sound interesting. In 1998 Warner Bros. bought the U.S. rights to the Japanese Pokémon cartoon series, based on the disgustingly popular Nintendo video-game characters. Anyway, since the TV show was such a successful electronic babysitter, Warner Bros. thought they should also import the incomprehensible Pokémon animated movies from the same country. To make the first movie, ironically and threateningly titled Pokémon: The First Movie, seem more American, Warner subsidiary Atlantic Records released a soundtrack featuring squeaky-clean teen acts like M2M singing "hip" songs that were usually relegated to one-minute excerpts over the film's end credits.
Well, since that was a big success, Warner Bros. thought they would do the exact same thing to the sequel, in this country titled Pokémon the Movie 2000: The Power of One (fortunately, we missed out on parts 2 through 1999). In addition to Donna Summer, the B-52s, and that dorky group from the show Popstars, our pal Weird Al was brought in to record a new polka all about those unstoppably annoying Pokémon critters. If you listen really hard, you can hear a snippet of Al's song, "Polkamon," over the end credits.
In early 2003, plans were made to rerelease the previous Al music-video DVD, "Weird Al" Yankovic: The Videos. For whatever reason, those plans were scrapped in favor this all-new, souped-up collection containing all of Al's music videos...and then some!
This new DVD includes all the music videos through "It's All About The Pentiums," the "Bob" video shot for 2003's Al-TV special, the Spy Hard title sequence (this time actually featuring two key on-screen titles!), Al and Jon's 1981 performance of "Another One Rides The Bus" from the old NBC Tomorrow Show, The Weird Al Show opening-theme sequence and the three music-video clips from the series, a cool photo gallery, and a very special easter egg that fits in with the disc's theme.
The videos themselves have been remastered and they both look and sound great (although some of the older videos may have an odd "tinny" sound to them depending on your DVD player's audio set-up). There's even on-screen lyrics and updated liner notes. As the title indicates, by definition this should be the end-all, be-all, final Weird Al music-video collection that will stand the test of time, and there's no reason why it isn't!
This page was last updated January 15, 2007.
"Weird Al" Yankovic: The Videos ©1997 Scotti Bros.
Desperation Blvd. ©1999 Desperation Blvd. Inc.
Pokémon the Movie 2000 ©1999, 2000 Nintendo/Warner Bros.


text:
Station Shin-Fukushima (新福島駅,  Shin-Fukushima-eki, Nieuw-Fukushima) is een treinstation in de wijk Fukushima-ku in de Japanse stad Osaka. Het wordt aangedaan door de JR Tozai-lijn. Het ligt naast het station Fukushima (Hanshin) en ten zuiden van het andere station genaamd Fukushima, welke door de Osaka-ringlijn wordt aangedaan. Het station heeft twee sporen, gelegen aan een enkel eilandperron.

Treindienst

JR West

Geschiedenis
Het station werd in 1997 geopend.

Overig openbaar vervoer
Bussen 39, 55 en 56

Stationsomgeving
 Station Fukushima voor de Hanshin-lijn
 Station Nakanoshima voor de Keihan Nakanoshima-lijn
 The Symphony Hall
 Hotarumachi (stadvernieuwingsproject)
 Kansai Denryoku-ziekenhuis
 Fukushima Tenmangū-schrijn
 Rihga Royal Hotel
 Raxa Osaka
 7-Eleven (2x)
 Sunkus
 Kantoor van Toyota

Shin-Fukushima

redpajama_set_name: RedPajamaWikipedia


NASE Certification - Level II - The National Association of Speed and Explosion (NASE) Inc.
This course requires the student to integrate knowledge learned from professional experience and prior learning in coaching and speed improvement. It will include appropriate discussions of muscle physiology, growth and development, and the energy systems as they relate to performance enhancement with an emphasis on speed development, high-performance sports conditioning, and advanced sports nutrition. This course will review and implement speed improvement programs specific to a sport and an athlete. The course will discuss nutrition plans using basic sports nutrition for athletic performance and speed improvement training for all types of athletes.
The training techniques will include foundation training, speed-strength and power training, plyometrics, sports loading , speed endurance training, sprinting form and technique and sprint-assisted training. Students will perform program design implementation for a case study including program planning, periodization the actual design of a workout schedule and sample workouts in the pre-season, in-season, and post season periods for each students specialty area ( strength and conditioning coaches, middle, high school, college and pro coaches; youth sports coaches, physical therapist, athletic trainers, personal trainers, undergraduates and graduate health and wellness, and Physical education and athletic training majors).
The students will document progress of their case study in speed improvement based on their client, profession, and sport at the end of the semester in the form of a written case study project. The student will take the the National Association of Speed and Explosion's Speed and Explosion Specialists credentialing exam as the Final Exam.
Demonstrate an understanding of the characteristic, training limitations and contraindications of athletes at various stages of growth and development.
Demonstrate an understanding of the effects of various training programs on muscle fiber types.
Identify and explain common kinetic chain dysfunction's as they relate to integrated, functional performance and rehabilitation/reconditioning.
Gain experience in diagnosing weaknesses and prescribing training programs to correct those weaknesses through the analysis of test scores.
Demonstrate an understanding of the foundation training programs that prepare an individual for high intensity speed improvement.
Demonstrate an understanding of the concepts and principals of the key training programs used to improve speed in short distances.
Prepare speed improvement programs specific to a sport and athlete in various positions within a sport.
Discuss and demonstrate an understanding of basic sports nutrition, recovery nutrition for speed improvement training, and safe muscle weight gain and weight loss practices.
In this assignment students will use themselves or a client to demonstrate their estimation of fast twitch fibers by finding their 1RM (one repetition maximum) for the double leg press, double leg extension, and the double leg curl. They will then take 80% of their one rep max for each test, complete as many repetitions as possible until muscle failure is achieved (can not do anymore repetitions). Students will refer to the chart (Charting Fiber Types) to locate their score on fiber typing.
1. What sport or skill is being assessed?
2. Why are the measurements important?
3. Where am I in growth and development (chronological or performance age)?
4. When and how often will my measurements be taken?
5. How will the measurements be collected and used?
Students will refer to the text for examples and design a functional Strength and power program.
1. What is plyometric training?
2. Why do we use this form of training?
3. What is sport loading?
4. How would you define speed endurance training?
Students will start thinking about a final project of developing a periodized sport specific speed program based on the sport they select. The project will be due by the end of the course and will be a 4 week program.
For this assignment students are required to write an applied paper. Students are to choose on the areas listed below. Students will review the literature, summarize the topic of choice and complete a two page written report of their findings. Only research based articles are permitted. The objective of the assignment is to research and report findings on a common performance enhancement aid or method for sprinters.
Below, is a list of some potential topics. You can use the readings from the module or the recommended readings for further ideas or resources. Don't forget that the references for these articles may also serve as more in depth resources for you.
Dintiman, G. & Ward, B. (2009). Encyclopedia of Sports Speed: Improving playing speed for sports competition. The National Association of Speed and Explosion. Kill Devil Hills, NC.
Enrollment for the NASE-SES Advanced Speed and Explosion Credential Exam.
All assigned readings will be available on the web if not in the required text.
Each module will require the student to read the required materials and then respond in a written assignment. Students must post an introduction of themselves and course evaluation.


text:
New BOV Chair and Co-Chair
Effective December 4, 2014 at the winter meeting of the Board of Visitors (BOV), Barbara O'Neal Eddleman becomes the BOV's 10th Chair. Joining her in leading the Board in the Co-Chair role is Dr. Douglas C. "Doug" Tilt, a BOV member since 2007.
Coming to the Chair post after two years as Co-Chair, Barbara believes in the BOV's ability to make good things happen. "As BOV members at this particular time, we have a four-star opportunity to serve this UAB School of Nursing that is really making a difference," she said. "We can provide support that can be a win-win-win for everyone involved –the School's students, its faculty and staff, and people of this state."
Doug is a physician with a long track record as a primary care leader –all the way from UAB to the Middle East. Excited about the UAB School of Nursing's current primary care initiatives, he said, "This nursing school is helping to develop new templates for providing primary care to the underserved. There are many medically underserved Alabamians –living in rural areas and also in cities, including Birmingham."
Barbara, formerly a career woman in marketing and commercial real estate, also is a mom –of architect daughter Cameron. A BOV member since 2002, Barbara understands the joy of giving and of seeing generosity among those in her life. She is appreciative of UAB School of Nursing support given by her late husband, Emmet O'Neal, (who died in 2004), and by Emmet's family; two UAB nursing scholarships bear the O'Neal name. Since marrying businessman Bill Eddleman in 2010, Barbara has seen how Bill and his fellow Hill Crest Foundation leaders enjoy supporting UAB School of Nursing programs.
Doug retired in March from UAB, where he held the Eleanor E. Kidd Endowed Chair in Primary Care Medicine and was director of the UAB Health System's Camellia Medical Group. He and his artist wife Sandy have three daughters –pediatrician Lindsey, realtor Rebecca, and Alex, who has begun UAB nursing studies. A recent family addition, granddaughter Elliot, is the daughter of Lindsey and husband Nate. Within his own family, Doug has felt the gratification of giving; he and his brothers LeRoy and Kenneth established a scholarship at the UAB School of Nursing in memory of their nurse mother, Martha Fanning Tilt.
Barbara and Doug take the BOV reins after two years of BOV success under the leadership of Chair Robert E. "Bobby" Luckie, III –success that Bobby said "is a credit to dedicated Board members, Dean Doreen Harper's leadership, and fine support from the School's faculty and staff."
Expressing confidence in new BOV leadership, Bobby said, "Barbara and Doug will be great leaders of this Board, no doubt about it. They are capable and compassionate people."
Read 7570 times	Last modified on October 24, 2017
Campaign for UAB

redpajama_set_name: RedPajamaCommonCrawl


This might sound bizarre, but you are likely familiar with a more extreme example of this: trauma. Whether it be in your own life or someone you know, it's all too easy to see the link between a traumatic boundary violation and the body's ability to remember and "record" this violation in the form of tension, illness, hypersensitivity to touch, and so forth.
But like any change, you have to actually practice it and live it, not just read and think about it. Therapy is an excellent tool for unlearning unhelpful boundary patterns and learning new ways of relating to yourself and others.


text:
layout:     post
title:      "SQL database in python"
subtitle:   "use mysql and xxx"
date:       2017-10-12
author:     "Ziping"
header-img: "img/python.jpg"
catalog: true
tags:
    - python
    - mysql
---

This blog is to record my process to connect mysql database in python.

I choose MySQLdb as my tool because it is said that MySQLdb is the most stable way to connect to a MySQL database.

MySQLdb doesnot support Python3 because I got an error:

```python
$ sudo pip install MySQL-python
Collecting MySQL-python
  Downloading http://mirrors.aliyun.com/pypi/packages/a5/e9/51b544da85a36a68debe7a7091f068d802fc515a3a202652828c73453cad/MySQL-python-1.2.5.zip (108kB)
    100% |████████████████████████████████| 112kB 637kB/s
    Complete output from command python setup.py egg_info:
    sh: mysql_config: command not found
    Traceback (most recent call last):
      File "<string>", line 1, in <module>
      File "/tmp/pip-build-TmLXPF/MySQL-python/setup.py", line 17, in <module>
        metadata, options = get_config()
      File "setup_posix.py", line 43, in get_config
        libs = mysql_config("libs_r")
      File "setup_posix.py", line 25, in mysql_config
        raise EnvironmentError("%s not found" % (mysql_config.path,))
    EnvironmentError: mysql_config not found

    ----------------------------------------
Command "python setup.py egg_info" failed with error code 1 in /tmp/pip-build-TmLXPF/MySQL-python/

# use this
conda install mysql-connector-python
```

The config file missing here is cause by ``ConfigParser`` that has changed in python3.

There is a replacement in Python3, ``pymysql``

The following is a simple case for fetching data.

```shell
pip install pymysql
```

```Python
#coding=utf-8

import pymysql as MySQLdb

host 	= "xxxx"
db 		= "xxxx"
user 	= "xxxx"
port 	= "xxxx"
passwd 	= "xxxx"

class SelectMySQL(object):
    def select_data(self,sql):
        result = []
        try:
            conn = MySQLdb.connect(host=host,
                               port=port,
                               user=user,
                               passwd=passwd,
                               db=db,
                               charset='utf8', )
            cur = conn.cursor()
            cur.execute(sql)
            alldata = cur.fetchall()
            # print(alldata)
            for rec in alldata:
                result.append(rec[0])
        except Exception as e:
            print('Error msg: ' + e)
        finally:
            cur.close()
            conn.close()

        return result

    def get_result(self, sql, filename):
        print(sql)
        results = self.select_data(sql)
        print('The amount of datas: %d' % (len(results)))
        with open(filename, 'w') as f:
            for result in results:
                f.write(str(result) + '\n')
        print('Data write is over!')
        return results

if __name__ == '__main__':
    sql = "select name from user"
    select = SelectMySQL()
    result1 = select.get_result(sql,'namemsg.txt')
    print(result1)
```

add your sql command.

## Create and Insert Table

It's important that you should begin and commit a transection when you have to write.

```python
conn = MySQLdb.connect(host=host,
                   port=port,
                   user=user,
                   passwd=passwd,
                   db=db,
                   charset='utf8')
conn.begin()
cur = conn.cursor()
create_table = """
use alpha;
DROP TABLE IF EXISTS xzp_alpha_id;
CREATE TABLE xzp_alpha_id (
    secID VARCHAR(20),
    date VARCHAR(10),
    value DOUBLE
);

INSERT INTO xzp_alpha_id (secID, date, value)
VALUES ('603152', '20170921', null);
"""
conn.commit()
cur.execute(create_table)
cur.close()
conn.close()
```

## MySQL Data Types

In MySQL there are three main data types: text, number, and date.

### Text data types:

| Data type        | Description                              |
| ---------------- | ---------------------------------------- |
| CHAR(size)       | Holds a fixed length string (can contain letters, numbers, and special characters). The fixed size is specified in parenthesis. Can store up to 255 characters |
| VARCHAR(size)    | Holds a variable length string (can contain letters, numbers, and special characters). The maximum size is specified in parenthesis. Can store up to 255 characters. **Note:** If you put a greater value than 255 it will be converted to a TEXT type |
| TINYTEXT         | Holds a string with a maximum length of 255 characters |
| TEXT             | Holds a string with a maximum length of 65,535 characters |
| BLOB             | For BLOBs (Binary Large OBjects). Holds up to 65,535 bytes of data |
| MEDIUMTEXT       | Holds a string with a maximum length of 16,777,215 characters |
| MEDIUMBLOB       | For BLOBs (Binary Large OBjects). Holds up to 16,777,215 bytes of data |
| LONGTEXT         | Holds a string with a maximum length of 4,294,967,295 characters |
| LONGBLOB         | For BLOBs (Binary Large OBjects). Holds up to 4,294,967,295 bytes of data |
| ENUM(x,y,z,etc.) | Let you enter a list of possible values. You can list up to 65535 values in an ENUM list. If a value is inserted that is not in the list, a blank value will be inserted.**Note:** The values are sorted in the order you enter them.You enter the possible values in this format: ENUM('X','Y','Z') |
| SET              | Similar to ENUM except that SET may contain up to 64 list items and can store more than one choice |

### Number data types:

| Data type       | Description                              |
| --------------- | ---------------------------------------- |
| TINYINT(size)   | -128 to 127 normal. 0 to 255 UNSIGNED*. The maximum number of digits may be specified in parenthesis |
| SMALLINT(size)  | -32768 to 32767 normal. 0 to 65535 UNSIGNED*. The maximum number of digits may be specified in parenthesis |
| MEDIUMINT(size) | -8388608 to 8388607 normal. 0 to 16777215 UNSIGNED*. The maximum number of digits may be specified in parenthesis |
| INT(size)       | -2147483648 to 2147483647 normal. 0 to 4294967295 UNSIGNED*. The maximum number of digits may be specified in parenthesis |
| BIGINT(size)    | -9223372036854775808 to 9223372036854775807 normal. 0 to 18446744073709551615 UNSIGNED*. The maximum number of digits may be specified in parenthesis |
| FLOAT(size,d)   | A small number with a floating decimal point. The maximum number of digits may be specified in the size parameter. The maximum number of digits to the right of the decimal point is specified in the d parameter |
| DOUBLE(size,d)  | A large number with a floating decimal point. The maximum number of digits may be specified in the size parameter. The maximum number of digits to the right of the decimal point is specified in the d parameter |
| DECIMAL(size,d) | A DOUBLE stored as a string , allowing for a fixed decimal point. The maximum number of digits may be specified in the size parameter. The maximum number of digits to the right of the decimal point is specified in the d parameter |

### Date data types:

| Data type   | Description                              |
| ----------- | ---------------------------------------- |
| DATE()      | A date. Format: YYYY-MM-DD**Note:** The supported range is from '1000-01-01' to '9999-12-31' |
| DATETIME()  | *A date and time combination. Format: YYYY-MM-DD HH:MI:SS**Note:** The supported range is from '1000-01-01 00:00:00' to '9999-12-31 23:59:59' |
| TIMESTAMP() | *A timestamp. TIMESTAMP values are stored as the number of seconds since the Unix epoch ('1970-01-01 00:00:00' UTC). Format: YYYY-MM-DD HH:MI:SS**Note:** The supported range is from '1970-01-01 00:00:01' UTC to '2038-01-09 03:14:07' UTC |
| TIME()      | A time. Format: HH:MI:SS**Note:** The supported range is from '-838:59:59' to '838:59:59' |
| YEAR()      | A year in two-digit or four-digit format.**Note:** Values allowed in four-digit format: 1901 to 2155. Values allowed in two-digit format: 70 to 69, representing years from 1970 to 2069 |

[//]: #	"host = rm-2ze3gjtcm507w8vqto.mysql.rds.aliyuncs.com; dbname = alpha; user = xu.zp; pwd = xzpDeepX"

redpajama_set_name: RedPajamaGithub


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text:
\section{Introduction}

One of the great, unanticipated legacies of the {\it Far Ultraviolet
Spectroscopic Explorer} (FUSE) mission is surely the detection of
\OVI\ absorption lines along extragalactic sight lines from the
warm-hot intergalactic medium (WHIM) at $T=10^{5-7}$~K, as predicted
by cosmological simulations \citep{CenOstriker99,Dave01}.  Hot gas in
the intergalactic medium (IGM) is produced by shocks generated by
gravitational instability during the formation of large-scale
structure, and its detection in highly ionized oxygen is an indicator
of widespread metal transport into the IGM through feedback from
galaxy formation.  The \OVI\ absorption probes gas at $10^{5-6}$~K,
somewhat cooler than the bulk of the WHIM, which has been shock-heated
to temperatures of several $\times10^6$~K.  This latter, very hot gas
is only detectable through weak X-ray absorption lines from higher
ions (e.g., \ion{O}{7}, \ion{O}{8}, \ion{Ne}{8}, \ion{N}{6},
\ion{N}{7}) as described recently by \citet{Nicastro05}.

The search for the WHIM gas has now begun in earnest, using sensitive
UV resonance absorption lines, primarily the \OVI\ doublet (1031.926,
1037.617~\AA) which is $\sim$100 times more sensitive than the X-ray
transitions of \ion{O}{7} (21.602~\AA) or \ion{O}{8}
(18.97~\AA). Thus, the initial WHIM detections of \OVI\ were made by
{\it FUSE} at $z\leq0.15$ and by the {\it Hubble Space Telescope}
(HST) at $z\geq0.12$, but over a modest total redshift pathlength
$\Delta z\approx0.5$ \citep{Tripp00,Savage02}.  For the portion of
WHIM containing \OVI, the estimated baryon fractions were $\sim$5\%
for O/H metallicity equal to 10\% of the former solar value,
$7.41\times10^{-4}$ \citep{Grevesse96}. Because the solar oxygen
abundance has recently been re-measured at
(O/H)$_{\odot} = 4.90 \times 10^{-4}$ \citep{abundanceref}, we have
re-scaled our baryon estimates to this lower value.  These estimates
have large uncertainties, including untested assumptions of uniform
metallicity, \OVI\ ionization equilibrium, and multiphase IGM
structure.

The initial \OVI\ searches reported only a handful of absorbers --
four systems by \citet{Tripp00} and six by \citet{Savage02}.  At low
redshift, down to 50~m\AA\ equivalent width in \OVI\ $\lambda1032$,
the number of \OVI\ absorbers per unit redshift is 10--15\% of that
found in the \HI\ \lya\ surveys: $d{\cal N}_{\rm OVI}/dz \approx
14^{+9}_{-6}$ \citep{Savage02} versus $d{\cal N}_{\rm HI}/dz \approx
112 \pm 9$ \citep{Penton4}.  In this study, we dramatically increase
the total surveyed pathlength to $\Delta z>2$ and the total number of
\OVI\ absorbers to 40.  We also study the relationship between
absorbers from the WHIM and the warm neutral medium (WNM;
$10^{3.5-4.5}$~K).  With the increased number of absorbers, we can
begin to look at WHIM absorption in a statistical manner, particularly
the distribution in \OVI\ column density.

\begin{figure*}
  \epsscale{1}\plottwo{f1a.ps}{f1b.ps}
  \caption{Comparison of H\,I and O\,VI column densities in 124 known
  \lya\ absorbers.  The left panel shows a mild correlation, if any,
  between \NHI\ and \NOVI.  While \NHI\ varies over a factor of nearly
  1000, \NOVI\ varies by a factor of only 20.  The right panel shows
  the ``multiphase ratio'', \NHI/\NOVI, with a dispersion of less than
  one dex over nearly three orders of magnitude in \NHI, suggesting
  that photoionized H~I and warm-hot gas occupy different phases of the
  IGM.  The multiphase ratio is well fitted by a power law,
  \NHI/\NOVI\ $= 2.5 \times
  [{\rm N}_{\rm HI}/10^{14}~{\rm cm}^{-2}]^{0.9 \pm 0.1}$
  (dashed line).  \NHI\ can be related to the overdensity,
  $\delta_H \equiv \rho/ \langle\rho\rangle$, as discussed in \S~4 and
  shown along the top axis.}
\end{figure*}

\section{Observations and Data Analysis}

We began our survey with published lists of intervening \lya\
absorption systems toward low-$z$ AGN obtained from GHRS and STIS
surveys by \citet{Penton1,Penton4}.  Other sight lines were covered by
literature sources or measured at the University of Colorado from
STIS/E140M spectra as discussed in the upcoming Danforth, Shull, \&
Rosenberg (2005, hereafter Paper~II).  We disregarded any weak \lya\
absorbers (W$_\lambda<80$~m\AA, log\,$N_{\rm HI}\la13.2$) and searched
the {\it FUSE} data for higher-order Lyman lines plus \OVI\ and \CIII\
counterparts. We have been conservative in our identification of
\OVI\ systems, requiring unambiguous ($\geq 4\sigma$) features, and
examining multiple channels of {\it FUSE} data and both lines of the
\OVI\ doublet when possible.  In all, we analyzed 171 absorbers in 31
{\it FUSE} sight lines.  We measured all available Lyman series lines
to determine accurate \NHI\ and doppler $b$ values for \HI\ via
curve-of-growth concordance curves \citep{Shull00}.

Of the \lya\ absorbers, 129 were at $z\leq0.15$, where \OVI\
absorption could potentially be observed.  We detected \OVI\ at
$4\sigma$ or greater level in one or both lines of the doublet for 40
absorbers, and we obtained $4\sigma$ or greater upper limits in 84
other cases.  The remaining five absorbers fell on top of airglow or
strong lines from the interstellar medium (ISM), were blended, or were
in some other way inaccessible.

We determined metal-ion column densities via Voigt profile fits and/or
the apparent column method \citep{SavageSembach91}. We assumed that
any saturation in these lines was mild, and that profile fits
accurately determine the column density.  In cases where we detected
both \OVI\ lines, we assigned a weighted mean of the column densities
to \NOVI.  We describe the full details of absorber selection and data
analysis in Paper~II.

\section{The Multiphase IGM}

The \OVI\ lines are ideal tracers (at $10^{5.5\pm0.3}$ K) for the
warm-hot ionized medium (WHIM; $10^5-10^7$~K), while \HI\ traces the
photoionized warm neutral medium (WNM; $10^{3.5-4.5}$~K).  The left
panel of Figure~1 shows a weak correlation, if any, between \NOVI\ and
\NHI.  While \NHI\ varies over nearly three orders of magnitude,
\NOVI\ is detected between $10^{13}$ cm$^{-2}$ and a few times
$10^{14}$ cm$^{-2}$ (a factor of $\sim$20).  To gauge the relative
amounts of warm photoionized gas (\HI) and hot collisionally ionized
gas (\OVI), we use the ``multiphase ratio'', \NHI/\NOVI. This ratio
was defined previously \citep{Shull03} as a means of assessing the
range in contributions from photoionized gas (\HI) and collisionally
ionized gas (\OVI), which often appear to be associated kinematically
\citep{Sembach03,Collins04}.

As shown in the right panel of Figure~1, the \NHI/\NOVI\ ratio
exhibits a strong correlation with \NHI, with a typical range
\NHI/\NOVI\ $\approx$ 0.5--50 and a dispersion of less than one (dex).
Higher \HI\ column absorbers typically display a higher multiphase
ratio, while weak \HI\ absorbers have $N_{\rm OVI} \approx
(0.1-2)N_{\rm HI}$.  We are well aware of the fact that plots such as
Figure~1 are subject to the effects of correlated errors in \NHI.
However, this ratio has physical utility in deriving a mean (O/H)
metallicity in multiphase gas (see \S~4), when combined with the empirical
correlation between \NHI\ and hydrogen overdensity, $\delta_H$, seen
in cosmological simulations \citep{Dave99}.

The large range in \NHI\ and the correlation in multiphase ratio
provide evidence that the IGM has at least two phases (WHIM and
WNM). If the \HI\ and \OVI\ materials were well mixed, we would expect
that the multiphase ratio would be constant with \NHI.  We suggest
instead that the WHIM occupies a shell around a warm neutral core.
The outer WHIM shell is heated by a combination of external ionizing
photons (from AGN), shocks from infalling clouds, and possible shocks
from cluster outflows such as superwinds and SNR feedback.  The narrow
range of \NOVI\ compared to \NHI\ implies that the WHIM shell may have
a characteristic column density of $10^{13}-10^{14}$ cm$^{-2}$, while
the neutral core can be arbitrarily large.

In this scenario, the very large values of the multiphase ratio
may arise in ``quiescent gas", possibly located in high-column
density H~I gas in halos.  The absence of associated \OVI\ suggests
the lack of shocks at velocities greater than about 150 \kms.
Many strong H~I (\lya) absorbers have been seen in
proximity (within $200h_{70}^{-1}$ kpc) of bright galaxies
\citep{Lanzetta95,Chen98,Penton3}.  In our current \OVI\ sample,
we found three absorbers with extremely high multiphase ratios: very
high neutral hydrogen columns with no detectable WHIM.  In the first
case, the absorber at $cz=1586$ \kms\ toward 3C\,273 shows
log\,$N_{\rm HI}=15.67$ and log\,$N_{\rm OVI}\leq13.17$ and is $71
h_{70}^{-1}$~kpc on the sky from a dwarf ($M_B = -13.9$)
post-starburst galaxy \citep{Stocke04}.  The second case is the
absorber at $cz=23,688$ \kms\ toward PHL\,1811 with log\,$N_{\rm
HI}=15.94$ and log\,$N_{\rm OVI}\leq13.06$.  This system is beyond the
$L^*$ survey depth, so we cannot comment on surrounding galaxies.
Finally, the Lyman-limit system at $cz=24,215$ \kms\ toward PHL\,1811
shows log\,$N_{\rm HI}=18.11$ and log\,$N_{\rm OVI}\leq13.06$.  This
absorber lies $23''$ ($34 h_{70}^{-1}$~kpc) from an $L^*$ galaxy at $z
= 0.0808$ \citep{Jenkins03}.  \citet{Tripp05} note a sub-DLA system at
$z_{\rm abs}=0.00632$ toward PG\,1216+069 with log\,$N_{\rm HI}=19.32$
and log\,$N_{\rm OVI}\leq14.3$ which lies 86 kpc from a sub-L$^*$
galaxy.  These four absorption systems, with multiphase ratios
log\,$[N_{\rm HI}/N_{\rm OVI}]\geq$ 2.5, 2.9, 5.0, and 5.0
respectively, may be shielded from external ionizing flux by adjacent
IGM clouds and have unshocked gas.

Metallicity is one of the great unknowns in interpreting the baryon
content of the WHIM absorbers.  In previous studies, (O/H) has been
assumed to be constant at 10\% solar.  However, one might expect that
metallicity variations could play a role in the multiphase ratio:
outflows of material from galaxies should be denser and more enriched
than primordial IGM clouds.  This would contribute a negative slope in
the multiphase ratio plot (Figure~1b).  Instead, the denser
(high-\NHI) absorbers show a relatively lower ratio of \OVI/\HI,
analogous to lower metallicity.  While metallicity variations almost
certainly exist in the IGM, they are not the main cause of the
positive slope in the multiphase ratio plot.  Some of this effect
could arise from changes in the mean \OVI\ ionization fraction,
typically chosen to be the maximum value, $f_{\rm OVI}\approx0.2$ at
$T_{\rm max}=10^{5.45}$~K in collisional ionization equilibrium
\citep{SutherlandDopita93}.  This fraction is expected to vary,
depending on the range of shock velocities that produce the \OVI\
\citep{Heckman02,Rajan05}.

\section{The Hot Baryon Content of the Universe}

\begin{figure}
  \epsscale{1.2}\plotone{f2.ps}
  \caption{Column density histogram for the observed O\,VI absorbers.
  Approximate equivalent widths for O\,VI $\lambda$1032 are shown
  along the top axis.  The decreasing number of absorbers at low
  column densities suggests that our survey is incomplete for weaker
  absorption lines.}
\end{figure}

Using \OVI\ as a tracer of the $10^{5-6}$~K portion of the WHIM, we
can employ the number of absorbers per unit redshift, $d{\cal N}_{\rm
OVI}/dz$, to determine $\Omega_{\rm WHIM}$, the fraction of the
critical density contributed by this WHIM gas.  Our detection
statistics are shown in Figure~2 for \OVI.

The total redshift pathlength of our survey is a function of
equivalent width, and our survey is more complete for strong absorbers
than for weak absorbers.  The equivalent-width sensitivity,
$W\rm_{min}(\lambda)$, is a function of spectrograph resolution,
$R=\lambda/\Delta\lambda$, and the signal-to-noise ratio (S/N) of the
data per resolution element.  Thus, for a $4\sigma$ detection limit,
we define $W_{\rm min}(\lambda)=4(\lambda/R)/(S/N)$.  We assume
$R=20,000$ and calculate $W_{\rm min}$ profiles for each dataset based
on S/N measured every 10 \AA.  Strong instrumental features, ISM
absorption, and airglow lines are masked out (S/N set to zero).  From
this procedure, we calculate $N_{\rm min}(\lambda)$ for both \OVI\
transitions, using curves of growth with $b_{\rm OVI} = 25$ \kms.  By moving
an absorber doublet along the profile as a function of $z_{\rm abs}$,
we generate a profile $N_{\rm min}(z)$.  By adding up the total path
length for each absorber at each $N_{\rm min}(z)$, we determine the
relationship between \NOVI\ and $\Delta z$ as shown in Figure~3.  With
a total high-$N_{\rm OVI}$ pathlength $\Delta z=2.21$, we are at least
80\% complete in \OVI\ detection down to log\,\NOVI\ = 13.4
($W_\lambda=30$~m\AA\ in the 1032 \AA\ line).  However, $\Delta z$ and
the completeness fall off rapidly for weaker absorbers.  Dividing
Figure~2 by Figure~3, we obtain the profile of $d{\cal N}_{\rm
OVI}/dz$ as a function of $N_{\rm OVI}$ (Figure~4).  To first order,
this procedure should correct for incompleteness in our \OVI\ survey.

\begin{figure}
  \epsscale{1.2}\plotone{f3.ps}
  \caption{Cumulative {\it FUSE} redshift pathlength, $\Delta z$, as
  function of 4$\sigma$ absorption-line detection limits in O\,VI
  column density and $\lambda1032$ equivalent width.  Strong lines can
  be detected in poor-quality data. Weak lines can only be detected in
  the highest-S/N observations and thus contribute less total path
  length.  We use the $\Delta z$ profile to correct for incompleteness
  in our O\,VI survey.}
\end{figure}

\begin{figure}[b]
  \epsscale{1.2}\plotone{f4.ps}
  \caption{Number of O\,VI absorbers per column density bin per unit
  redshift after our first-order completeness correction.  Even after
  this correction, the number of O\,VI absorbers appears to fall off
  rapidly below log\,\NOVI $\leq 13.4$.  However, the statistics are
  poor with only five absorbers in the lowest two bins.}
\end{figure}

Our incompleteness-corrected value of the absorber frequency, $d{\cal
N}_{\rm OVI}/dz$, compares well with previous, uncorrected values
(Table~1).  For \OVI\ absorbers with $W_{\lambda} \geq 50$~m\AA\ (in
$\lambda 1032$), we find $d{\cal N}_{\rm OVI}/dz = 9\pm2$, somewhat
lower than the value, $d{\cal N}_{\rm OVI}/dz=14^{+9}_{-6}$, found by
\citet{Savage02} using six \OVI\ absorbers toward PG\,0953+415.
For the weaker \OVI\ absorbers, we find $d{\cal N}_{\rm OVI}/dz =
17\pm3$ ($\rm W_\lambda\geq30$~m\AA) and $d{\cal N}_{\rm OVI}/dz =
19\pm3$ ($\rm W_\lambda\geq15$~m\AA) from our total sample of
$40^{+7}_{-6}$ measured \OVI\ absorbers.  Uncertainties are based on
single-sided $1\sigma$ confidence limits in Poisson statistics
\citep{Gehrels86}.  \citet{Tripp00} found $d{\cal N}_{\rm OVI}/dz>17$
at 90\% confidence for $\rm W_\lambda\geq30$~m\AA, based on four
absorbers toward H1821+643.

A recent study \citep{Tripp04} using STIS/E140M data finds $d{\cal
N}_{\rm OVI}/dz=23\pm4$ for $\rm W_\lambda\geq30$~m\AA\ based on 44
\OVI\ absorbers.  This sample was taken at slightly higher redshift
($0.12\leq z_{\rm abs}\leq0.57$) than our sample ($z_{\rm abs}\leq
0.15$) and shows a higher value of $d{\cal N}_{\rm OVI}/dz$.  This is
not predicted by simulations, which predict an {\it increasing} WHIM
fraction at recent epochs.  However, the difference in redshift
between the two samples is small, and the discrepancy in $d{\cal
N}_{\rm OVI}/dz$ may be a result of cosmic variance.

\begin{figure}
  \epsscale{1.2}\plotone{f5.ps}
  \caption{Cumulative equivalent width distribution for O\,VI
  absorbers after Figure~10 of \citet{Chen03}.  Our data points
  (filled diamonds) at (O\,VI $\lambda1032$) equivalent width detection
  thresholds of 10, 15, 30, 50, and 100 m\AA\ are slightly lower than
  values from \citet{Savage02} (square), \citet{Tripp00} (circle), and
  \citet{Tripp04} (triangle).  Models from \citet{Chen03} show the
  simulated distribution at a range of metallicities: $Z=0.1Z_\odot$
  (solid curve), $Z=Z_\odot$ (dotted), and an overdensity-dependent
  metallicity $Z=Z(\delta_{\rm H})$ (dashed).  The $Z=0.5\,Z_\odot$ model
  used by \citet{Fang02} (dot-dashed) represents a more simplified
  physical model.}
\end{figure}

Recent cosmological simulations of the X-ray forest predict a
distribution of \OVI\ absorbers and provide a convenient way to check
current simulations with observed data.  \citet{Chen03} model the
X-ray forest assuming a $\Lambda$CDM model similar to \citet{Dave01},
both collisional ionization and photoionization from a UV background,
radiative cooling, and a range of different metallicities.  The cumulative
distribution of \OVI\ absorbers ($d{\cal N}_{\rm OVI}/d{\rm ln}[1+z]$)
down to a minimum equivalent width is drawn from these models
and provides a convenient comparison with observed statistics
from our work and previous surveys (see Figure~5).

The simulation with $Z=0.1\,Z_\odot$ shows a reasonably good match to
the observed cumulative distribution of \OVI\ absorbers in the local
universe.  Weaker absorbers ($W_\lambda<30$ m\AA) are overpredicted
compared with observations, but this may be a matter of small-number
statistics or differing detection thresholds between observations and
simulations.  A simulation in which metallicity is a function of
overdensity fits the data slightly better than the fixed-metallicity
model.  However, \citet{Chen03} caution that there is a substantial
scatter in the simulations, so that the lower-metallicity curves are
essentially indistinguishable.  The $Z=0.5\,Z_\odot$ model of
\citet{Fang02} also fits the observed data reasonably well, but it is
based on a less physical simulation with no photoionization and no
radiative cooling.  The solar metallicity model of the IGM can clearly
be ruled out by our observations.  Simulations at lower metallicities
($Z = 0.01\,Z_\odot$) would be helpful, given the wealth of new
observational results.

\begin{deluxetable}{lcccl}
\tabletypesize{\footnotesize}
\tablecolumns{5}
\tablewidth{0pt}
\tablecaption{IGM O\,VI Absorber Statistics}
\tablehead{\colhead{Criteria}        &
           \colhead{${\cal N}_{\rm abs}$}  &
	   \colhead{$d{\cal N}/dz$}  &
           \colhead{$\Omega_{\rm WHIM}$\tablenotemark{a}} &
	   \colhead{reference} }
\startdata
 $W\geq10$  m\AA&  40 & $21\pm3$        &  $0.0022\pm0.0003$ & this work \\
 $W\geq15$  m\AA&  38 & $19\pm3$        &  $0.0021\pm0.0003$ & this work \\
 $W\geq30$  m\AA&  35 & $17\pm3$        &  $0.0021\pm0.0004$ & this work \\
 $W\geq50$  m\AA&  19 & $~9\pm2$        &  $0.0016\pm0.0005$ & this work \\
 $W\geq100$ m\AA&   6 & $~3^{+2}_{-1}$  &  $0.0008\pm0.0004$ & this work \\
                &     &                 &                    &            \\
 $W\geq30$  m\AA&  44 & $23\pm4$        &  0.0027 & \citet{Tripp04} \\
 $W\geq30$  m\AA&   4 & $>17~~~$        & $>$0.006\tablenotemark{b}& \citet{Tripp00} \\
 $W\geq50$  m\AA&   6 & $14^{+9}_{-6}$~~&$\geq$0.003~~~& \citet{Savage02}
\enddata
\tablenotetext{a}{All $\Omega_{\rm WHIM}$ values have been converted to a consistent set of assumptions:  $f_{\rm OVI}=0.2$, $Z=0.1\,Z_\odot$, $H_0=70h_{70}~{\rm km~s^{-1}~Mpc^{-1}}$, and (O/H)$_\odot=4.9\times10^{-4}$ \citep{abundanceref}.}
\tablenotetext{b}{All four O\,VI absorbers in \citet{Tripp00} lie along the unusually rich H1821+643 sight line.}
\end{deluxetable}

From $d{\cal N}/dz$, we can calculate the contribution to $\Omega_b$
from WHIM gas, as discussed in \citet{Savage02}.  We assume a Hubble
constant $H_0=70 h_{70}$ \kms~Mpc$^{-1}$, rather than their value
$h_{75}$, and we make standard assumptions regarding \OVI\ ionization
fraction and (O/H) metallicity \citep{Tripp00,Savage02}.  We adopt an
ionization fraction, $f_{\rm OVI}=0.2$ characteristic of its maximum
value in collisional ionization equilibrium (CIE) and assume an O/H
abundance 10\% of the solar value.  Of course, CIE is almost certainly
not a valid assumption for the low-density IGM.  As the infalling gas
is shock-heated during structure formation, the ionization states
\OVI, \ion{O}{7}, and \ion{O}{8} undergo transient spikes in
abundance, followed by cooling and recombination.  Recent
time-dependent models of the ionization, recombination, and cooling of
shock-heated, low-density WHIM \citep{Rajan05} find that the mean,
time-averaged \OVI\ ion fraction is $\langle f_{\rm OVI}
\rangle=$8--35\%, over a range of initial temperatures $5.4 \leq
\log T \leq6.2$.  These fractions are compatible (with a factor of two
spread) with the fiducial value, $f_{\rm OVI} = 0.2$, based on the
maximum fraction of \OVI\ at $T_{\rm max} = 10^{5.45}$~K, in CIE
\citep{SutherlandDopita93}.

As shown above (Fig.\ 5), a metallicity $Z=0.1\,Z_\odot$ is reasonably
consistent with the observed equivalent width distribution of \OVI\
absorbers at $z\sim0$. However, using our sample of \OVI\ and \HI\
absorbers, we can make a more direct estimate of the (O/H) metallicity.
To do so, we must estimate the amount of hydrogen associated with
each component of the the multiphase system of photoionized \HI\ and
collisionally ionized \OVI.  Since the \HI\ and \OVI\ absorbers are
associated kinematically, we assume they share the same metallicity.
We then use the empirical relations between \NHI\ and overdensity,
$\delta_H$, and between the multiphase ratio (\NHI/\NOVI) and \NHI.

\begin{equation}
   \left( \frac {N_{\rm HI}} {N_{\rm OVI}} \right) = C_0~N_{14}^{\alpha} \; ,
\end{equation}
and
\begin{eqnarray}
   \delta_{\rm H} &\equiv& \frac {n_H} {(1.90 \times 10^{-7}~{\rm cm}^{-3})(1+z)^3}\nonumber \\
                  &\approx& 20~N_{14}^{0.7}~10^{-0.4z}   \; .
\end{eqnarray}
The above relations allow us to relate \NHI\ to the physical gas density,
$n_H$, needed for the hydrogen photoionization correction.
Equation (1) is derived by fitting the multiphase correlation
in Fig.\ 1b over the approximate range $10 \leq \delta_{\rm H} \leq 300$.
The scaling constant $C_0 = 2.5 \pm 0.2$ is the mean multiphase ratio
at log\,\NHI\ = 14, and the best-fitting slope is $\alpha = 0.9\pm 0.1$.
Equation (2) comes from cosmological simulations \citep{Dave99}
and relates the hydrogen overdensity, $\delta_H$, to the \HI\ column
density, N$_{\rm HI} \equiv (10^{14}~{\rm cm}^{-2}) N_{14}$.

From these relations, we can derive a statistical value of the
(O/H) metallicity from the formula,
\begin{equation}
     \langle N_{\rm O}/ N_{\rm H} \rangle =
          \langle N_{\rm OVI}/ N_{\rm HI} \rangle
         \times \left( \frac {f_{\rm HI}} {f_{\rm OVI}} \right) \; .
\end{equation}
We employ the multiphase ratio, \NHI/\NOVI, together with appropriate ionization
correction factors, $f_{\rm OVI}$ and $f_{\rm HI}$.
The \HI\ fraction is derived from photoionization equilibrium in
the low-$z$ IGM
\begin{equation}
   f_{\rm HI} = \frac {n_e \alpha_H^{(A)}} {\Gamma_H} =
      (1.80 \times 10^{-5}) (1+z)^3 \left( \frac {\delta_H}{20} \right)
      T_4^{-0.726} \Gamma_{-13}^{-1}  \; ,
\end{equation}
for gas with $n_e = 1.16 n_H$ at temperature $(10^4~{\rm K})T_4$,
photoionized at rate $\Gamma_{\rm H} = (10^{-13}~{\rm s}^{-1})
\Gamma_{-13}$.  Since the mean-free path of a Lyman continuum photon
is very large in the low-overdensity IGM, we use the case-A
recombination rate coefficient $\alpha_H^{(A)} = (4.09 \times
10^{-13}~{\rm cm}^3~{\rm s}^{-1}) T_4^{-0.726}$.  Combining the two
empirical relations with the relation of photoionization equilibrium,
we find that the mean oxygen metallicity of the
\OVI\ absorbers at $\langle z \rangle = 0.06$ is
\begin{equation}
   Z_{\rm O} = (0.09 Z_{\odot}) N_{14}^{-0.2} T_4^{-0.726} \Gamma_{-13}^{-1}
     \left( \frac {f_{\rm OVI}} {0.2} \right)^{-1}   \; .
\end{equation}
Given the uncertainties in these empirical relations, it is remarkable that
this formula arrives at an oxygen abundance near the fiducial value of 10\%
solar.   In fact, our estimated value, $Z_{\rm O} = 0.09 Z_{\odot}$, is
probably accurate to only a factor of 2.

\newpage
We now derive the fractional contribution to closure density of WHIM
baryons associated with hot \OVI,
\begin{eqnarray}
\Omega_{\rm WHIM}&=&\left(\frac {H_0} {c\,\rho_{\rm cr}}\right) \frac{\mu m_H}{(O/H)_{\odot}~Z~f_{\rm OVI}}\nonumber \\
&&\times\int_{N_{\rm min}}^{N_{\rm max}}\left(\frac{d\cal{N}}{dz}\right)\,\langle N_{\rm OVI}\rangle\,dN_{\rm OVI} \\
&=&(1.85\times10^{-18})~h^{-1}_{70}~\sum_i\left(\frac{d\cal{N}}{dz}\right)_i\;\langle N_{\rm OVI}\rangle_i\;.\nonumber
\end{eqnarray}
We perform the above sum using the value, $(d{\cal N}/dz)_i$, for each
column-density bin in Figure~4, with $\langle N_{\rm OVI}\rangle_i$
chosen as the mean column density (cm$^{-2}$) in the bin.  We find
$\Omega_{\rm WHIM} = (0.0022\pm0.0003) h_{70}^{-1}$.  Values of
$\Omega_{\rm WHIM}$ for other equivalent width thresholds are listed
in Table~1 along with the results of other studies converted to
uniform values of $H_0$, $f_{\rm OVI}$, and (O/H)$_{\odot}$.

It should be stressed that these estimates of $\Omega_{\rm WHIM}$ are based
on an assumed uniform 10\% solar (O/H) metallicity and that further
uncertainty arises in our assumed \OVI\ ionization fraction.  Changes
in $f_{\rm OVI}$ within the range of mean values \citep{Rajan05} could
change our result by a factor of two.  Based on the standard
assumptions, our result is slightly lower than the result published by
\citet{Savage02}, $\Omega_{\rm WHIM}\geq0.002 h_{75}^{-1}$.
\citet{Savage02} used an older solar oxygen abundance, (O/H)$_\odot =
7.41\times10^{-4}$, which is 50\% larger than the \citet{abundanceref}
value.  After correcting for this difference, their result for
$\Omega_{\rm WHIM}$ is larger than ours.  \citet{Tripp04} find
$\Omega_{\rm WHIM}=0.0027$ based on 44 absorbers at $z\geq0.12$.

Our estimate corresponds to $\Omega_{\rm WHIM}/\Omega_b = 0.048\pm 0.007$,
so that WHIM gas in the range $10^{5-6}$~K makes up roughly 5\% of the
baryonic mass in the local universe.  The contribution could exceed 10\%
if we account for the likely spread in (O/H) metallicities and \OVI\
ionization fractions.  Simulations predict that the current universe is
composed of $\sim30$\% WHIM gas, so our value of $\sim3-10$\% falls
short of this mark.  However, \OVI\ is only useful as a proxy for gas
within the lower portion of the WHIM temperature range.  Accounting for
the hotter $10^{6-7}$~K gas using similar methodology will require
high-sensitivity, high resolution X-ray observations of \ion{O}{7} and
\ion{O}{8} with spectrographs aboard future missions such as Constellation-X
or XEUS \citep{Fang02,Chen03}.  Limited observational work has been done in
this area \citep{Nicastro05}, but the current generation of X-ray
telescopes are not ideal for this kind of investigation.

The distribution of \HI\ absorbers with column density is often
expressed as a power law with index $\beta$: $d{\cal N}/dN \propto
N^{-\beta}$ \citep{Weymann98,Penton2,Penton4}.  For the first time,
this analysis can be applied to WHIM species.  We find that the
differential number of \OVI\ absorbers with column density is a power
law, $d{\cal N}_{\rm OVI}/dN_{\rm OVI} \propto N_{\rm
OVI}^{-2.2\pm0.1}$ for absorbers with log\,$N_{\rm OVI}\geq13.4$.
This is somewhat steeper than the corresponding \HI\ distribution,
$\beta\sim1.6$ \citep{Penton4} and means that low-column absorbers
contribute comparable amounts to the \OVI\ baryon census as the rare
high-column systems.  Note that in eq.~[6], $\Omega_{\rm WHIM}$ scales
as $N_{\rm min}^{-0.2}$ for $\beta=2.2$.  Even though we correct for
incompleteness in the weaker absorbers, the statistics are still poor
at log $N_{\rm OVI}\leq13.4$.  It is unclear whether the turnover in
$d{\cal N}_{\rm OVI}/dz$ at lower columns is real or a statistical
fluctuation from small numbers of weak absorbers.  Nevertheless, the
weak \OVI\ absorbers appear to make significant contributions to the
baryon mass density.  The steep power law also reinforces our
conclusions about the nature of the multiphase IGM with a core-halo
structure.

We have demonstrated that the contributions from weak \OVI\ absorbers
cannot be neglected in an accurate WHIM baryon census.  The rare
strong \OVI\ absorbers and numerous weak absorbers contribute nearly
equally to $\Omega_{\rm WHIM}$.  Further FUSE observations at high-S/N
will allow us to probe weak \OVI\ absorbers and refine the statistics
at the low-column end of the absorber distribution.  An analysis of
\OVI\ absorbers at higher redshifts ($z>0.5$) would allow us to track
changes in the WHIM density, confirming the decrease in the amount of
shocked gas at higher redshifts predicted by cosmological simulations
\citep{CenOstriker99,Dave99,Dave01}.

Only by enlarging our sample of multiphase (\HI, \OVI) absorbers
beyond the 40 discussed here will we be able to refine our statistical
estimate for the metallicity of the WHIM.  With a much larger sample
of \OVI\ absorbers, we could use maximum-likelihood techniques to
search for the expected trends: (1) decreasing metallicity at lower
overdensity $\delta_H$ \citep{Gnedin97}; (2) decreasing $\Omega_{\rm
OVI}$ at higher redshift \citep{Dave99}; and (3) trends of \NHI/\NOVI\
with other metal indicators such as \CIII, \ion{C}{4}, or \ion{Si}{4}.

\acknowledgments

We are grateful to Steve Penton, John Stocke, Jessica Rosenberg, Todd
Tripp, Bill Blair, Blair Savage, Ken Sembach, and Jason Tumlinson for
useful discussions regarding this project.  This work contains data
obtained for the Guaranteed Time Team by the NASA-CNES-CSA {\it FUSE}
mission operated by the Johns Hopkins University, as well as data from
the {\it Hubble Space Telescope}.  Financial support to the University
of Colorado has been provided by NASA/{\it FUSE} contract NAS5-32985
and grant NAG5-13004, by our HST \lya\ survey program 6593, and by
theoretical grants from NASA/LTSA (NAG5-7262) and NSF (AST02-06042).

redpajama_set_name: RedPajamaArXiv


text:
Home Real Estate Slayer guitarist Kerry King rocks into $3.6 M Tribeca crib
Slayer guitarist Kerry King rocks into $3.6 M Tribeca crib
He slayed the deal!
Thrash metal guitarist Kerry King — who was the lead guitarist for Slayer and collaborated with Megadeth — and his wife, Ayesha, just plunked down $3.65 million on a Tribeca triplex.
It was last asking $3.92 million.
King — who recently said Slayer retired "too early" — also worked on the song "License to Ill" and "No Sleep till Brooklyn" with the Beastie Boys.
Ayesha announced the move back to the Big Apple on her Instagram, saying New York is "back home for me, excited to be near my family again."
The renovated two-/three-bedroom unit is at 12 Warren St., a boutique condo built in 2016.
It was on the market for 45 days and comes with $4,572 monthly common charges.
Seasons in the a-bliss: One of the home's plurality of bedrooms.
The triplex lives at 12 Warren St. in Tribeca.
Tamara Beckwith
At 3,522 square feet, the spacious digs open to a foyer and ceilings run as high as 22 feet 7 inches.
The main floor boasts an open chef's kitchen that leads to a dining room.
There's 3,522 square feet of space inside the Tribeca home.
The smart-wired home also features wide-plank white oak floors and a home theater.
An open chef's kitchen leads into the dining room.
The couple have been on a bit of a pandemic real estate buying roll. In 2020, they also bought a $3.8 million home in Las Vegas Valley, Nev., according to reports.
The listing brokers for the New York City triplex were Shea Mena and Chris Fry of Elegran.
The Connection Between Visualization and Motivation
One chef finds silver lining in COVID lockdown
Business Washington Herald - January 4, 2022
Apple, Vipshop, Coinbase and others
Moderna, Zynga, Lululemon, Tilray and more
Markets Washington Herald - January 10, 2022


text:
Gift Cards & Rewards
Online ordering now available! Click here.
Textbox Section
Gift Cards/Rewards
We are a family-owned and operated, farm-to-table style restaurant located just outside of Kalamazoo in Texas Township. Our belief is that craft beer deserves craft food! Our menu features fresh, made from scratch options available nowhere else. Beer and cider selections are 100% crafted by us. They include familiar beer styles, hard cider made from apples grown in our family's orchards, and experimental small batch brews. Join us for a wonderful food and beverage experience in our 100 year old historic church, now renovated into a beautiful tap room!
Photo by Encore Magazine/Brian Powers
Texas Corners Brewing Company was founded by the Schultz family of Mattawan. Entrenched in the local community with their family farm in since 1951, Bill and Denise looked to expand their operation into something less weather dependent than agriculture. With award winning traditional cider already being made, they made the foray into hard cider in 2013. Events snowballed quickly from there, when they purchased the former Christ the King church you are inside today. Operations expanded into craft beer and a full service farm-to-table restaurant when doors were opened in March of 2015.
All of the family is involved in the family business. Bill and Denise run the farm along with their sons Bill and Dan. The third son Andrew manages the restaurant where he met his wife Ruth. Their sister Robyn lives out of the state, but still comes home occasionally to help. Dan and his wife Audrey have even started the 4th generation with two young girls – Lena and Ahna.
Texas Corners Brewing Company is a homage to the family history which was started by grandparents Victor and Dorothy after WWII. A canvas near the bar is tribute to them. We look forward to providing quality craft beer, cider, and food at Texas Corners for a long time to come. After all, craft beer deserves craft food!
Growing up on the family farm in Mattawan, Andrew Schultz has always had an interest in food - from growing it, to manufacturing and marketing, to consuming it. Andrew focused on food while at Michigan State University where he graduated with a Bachelor's degree in Agribusiness Management. Working for a global food company in Texas, he decided to return to Texas Corners when the opportunity presented itself to start a new family business from scratch. Check out the menu to see what seasonal creations the team at TCBC have crafted!
Head Brewer
While traveling the world Jeremy found a passion for craft beer and starting creating his own at home around eight years ago. Growing up in Western Michigan with its abundance of agriculture, and studying mechanical engineering at Western Michigan University has been Jeremy's inspiration. He is dedicated to his community and incorporating the freshest, local ingredients possible in each of his brews. Check out our current tap list to see which of his creations you can try today!
Why is it called "Texas Corners" Brewing Company?
Texas Corners is the name of the intersection directly to the south of our restaurant. We are also located on the corner of 8th St. and Texas Drive. Our brewpub is located in Texas Township, which was founded and settled around the time Texas gained independence. It's believed locals took inspiration from the Texas independence movement. You can find out more on the history of the area at the Texas Charter Township website.
How long have we been open?
The building was purchased by our family in 2013 and our dream of a brewery and restaurant went into motion. Construction and licensing took about two years, and we officially opened to the public on March 23, 2015.
Was the building a church or a school house?
The original part of our restaurant and taproom was designed and built as a church during the 1910's. The front steeple portion was added at a later date, and the kitchen was added on right before we opened in 2015. The building was a church until the mid-1990's before being repurposed as a gift shop. At the time we purchased in 2013, the building had been abandoned, so we repurposed this historic building into a restaurant. At over 100 years old, it is one of the oldest standing buildings in the Texas Corners area.
What is the meaning of the apple in your logo?
TCBC started as an extension of our third generation family fruit farm – Schultz Fruitridge Farms. On the farm, apples are our number one crop, and making hard cider was the original inspiration for starting the brewery. 100% of the apples used in our hard cider are grown right on the family farm five miles away in Mattawan, MI.
Why a farm-to-table menu?
With our family's roots in farming that span over three generations, we believe that food that comes fresh from the farm can be picked at optimal ripeness, and therefore has optimal flavor. We also believe in supporting our local farming community. We use fresh fruits, vegetables, and proteins from our own farm, the local farmers' market, other area farmers, our community college food hub, and our foodservice distributor. We consider anything grown, raised, or produced in Michigan as local.
Why are you closed on Sundays?
We are a small, family-owned and operated business. We work in the restaurant daily and like all people we need some rest. Being closed Sundays helps us and our staff rest and recover to serve you at 100% the remainder of the week!
Where do you brew your beer and cider?
We have a small pilot brewing system in our restaurant's basement, but the majority of our production currently happens at our family farm, five miles west in Mattawan. We brew and cellar most of our beer and cider in our production facility there, before transferring to our pub in Texas Corners.
Why is your flagship India Pale Ale named "Three Brothers"?
There are three brothers in the Schultz family who own and run TCBC – Bill, Dan, and Andrew. Andrew is involved on a daily basis at the restaurant. Bill and Dan are farmers at the family farm, and grow all of the apples in our hard cider.
Why is your flagship porter named "P-51"?
Our grandfather Victor started the family farming business in 1951. Before that, he was a pilot for the US Army Airforce in WWII. He flew a campaign in North Africa and Southern Italy in a P-51 Mustang fighter. Without Victor's vision of starting the family farm after the war, no one in the family would be doing what we are doing today. The P-51 Porter was our first beer we brewed, and it's named in his honor.
Where can I find your brews?
Our brewery system is relatively small, so we sell 99% of our craft beers at our pub. The small remainder we sell to the occasional local bar or individual for parties. We do can and sell our hard cider at our pub, farm market, and about a dozen independent craft beer party stores in the greater Kalamazoo area.
Do you grow your own hops?
Yes, we have about two dozen Cascade and Centennial hop plants. We grow enough to brew 2-4 seasonal and small batch "harvest" ales. These brews are crafted with hops picked from our plants and used in the brewing process within days of harvest. Our remaining craft brews are crafted largely with Michigan-grown hops.
Be sure to check out our family's other local business.
Website Design by 2 Acre Studios
Texas Corners Brewing Company
6970 Texas Drive,
Mon-Thurs: 4-9 pm
Fri-Sat: 12-10 pm


text:
Q: I need to set a variable or return data from asynchronous javascript call I have the following functions...
    If(signInSet(sign_in_data)){
        do something... //appends data to a variable that is outputted after the if statement
    }
    else{
        do something else...
    }

Then...
   signInSet(sign_in_data){
      var equal = false;
      $.get('url', function(currentDate){
           $.each(sign_in_data, function compareDate(){
           if(this.date === currentDate){
                equal = true;
                return false;  //to end the each loop
           }
         });
          //at this point i can see and print out the value of equal
      });

Im have some knowledge of the asynchronous nature of this function, what im wondering is how i can refactor my code to be able to see the value of equal so i can use it in my if statement. thanks in advance.

redpajama_set_name: RedPajamaStackExchange


text:
23 Non-Food Places You May Find Hidden Peanuts
More in Food Allergies
Common Types
Children & Food Allergies
Jeanette Bradley
Jeanette Bradley is a noted food allergy advocate and author of the cookbook, "Food Allergy Kitchen Wizardry: 125 Recipes for People with Allergies"
Medically reviewed by Daniel More, MD on November 21, 2019
Daniel More, MD, FAAAAI, FACAAI, FACP, is a board-certified allergist and clinical immunologist with a background in internal medicine.
Daniel More, MD
Kryssia Campos / Getty Images
If you or a loved one has a peanut allergy, you're almost certainly accustomed to checking ingredient labels for peanut ingredients. But did you realize peanut-derived ingredients—ranging from peanut oil to shells—also can be found in multiple non-food items that range from cosmetics to cat litter.
In fact, peanuts crop up in some truly surprising places. This obviously isn't a problem if you're not allergic to them, but for those who are allergic (especially those who have a severe peanut allergy), these various uses in non-food items make the world a much more dangerous place.
Where Can You Find Peanuts?
It might not surprise you to run across peanuts in birdseed—in fact, you can probably even see them in the bag and know to stay away. Likewise, peanut shells and skins also are used to provide fiber roughage in livestock feed, so people who are allergic to peanuts should exercise caution if they need to handle feed used for livestock.
But what about cosmetics? While you wouldn't expect to find peanuts in your soap, shampoo or body lotion, peanut-derived ingredients are not uncommon in those products. You even can find peanut shells in artificial fireplace logs.
All in all, Verywell found 23 non-food products that can be made with peanuts.
Bear in mind that not all products on the following will definitely contain peanuts—in some cases, peanuts aren't currently used or have just been used in research projects. But this list should provide you with what you need to do your own due diligence in order to keep yourself (or your peanut-allergic loved one) safe.
Non-Food Items Possibly Containing Peanuts
Here are the various places that peanut shells or skins may possibly be used in non-food items:
Cat litter. Blue Buffalo brand's Blue Naturally Fresh cat litter used to be made from peanut shells but is currently made from walnut shells.
Paper. Although scientists have explored this, there don't seem to be any instances where it's being done commercially.
Stuffing for beanbags or stuffed animals. This doesn't appear to be common, but it crops up occasionally and is still something to watch out for. It's possible for homemade beanbag-style toys to use birdseed as their stuffing, which can contain peanuts.
Wallboard. Again, this isn't a common use for peanuts, but if your allergy is severe and you anticipate working with wallboard (or having work done in your home), you may want to double-check on the ingredients.
Artificial fireplace logs. These logs use "ground biomass," which can include ground-up peanut and tree nut shells.
Livestock feed.
Peanuts themselves may be ingredients in:
Axle grease. George Washington Carver first used peanuts for this purpose, although petroleum-based products are much more common these days.
Birdseed.
Bleach. This only applies to color-safe bleach varieties, not chlorine-based bleach.
Cosmetics. Here, you should look for ingredients with "Arachis Hypogaea," which is the scientific name for peanut.
Detergent. This is unusual, but it is possible to find peanuts in detergents.
Explosives. Peanuts can be used to make the explosive nitroglycerin.
Face creams. Again, as with cosmetics, look for "Arachis Hypogaea" on the product's label.
Ink. George Washington Carver started this, too, but it's not much found in the modern world.
Linoleum. This is yet another George Washington Carver invention.
Medicine. Always make sure to tell your pharmacist you're allergic to peanuts when filling a prescription, and double-check on any over-the-counter drugs you purchase.
Metal polish. Peanuts seem to be most common as an ingredient in homemade polishes.
Pet food. Dogs like the taste of peanut butter and several common dog treats come in peanut flavor.
Paint. This is a highly unlikely (but possible) use for peanuts.
Rubber. George Washington Carver experimented with this, but I couldn't find any evidence that it's ever been done commercially.
Shampoo. Once again, watch for those Arachis Hypogaea ingredients.
Shaving cream. Check for Arachis Hypogaea on the ingredients list.
Soap. Check for Arachis Hypogaea on the ingredients list.
As you can see, some of these places are far less likely than others—in fact, a good percentage of them likely never made it out of George Washington Carver's laboratory (which, let's face it, must have been a dangerous place for those with peanut allergy).
But other places peanuts can hide (pet food and cosmetics come to mind) are a much bigger risk.
So what can you do to stay safe if you or a loved one has a peanut allergy? Well, you need to keep in mind that peanuts can be found in more than just food items, stay vigilant, read ingredients labels, and call the manufacturer if there's any ambiguity.
Get one simple hack every day to make your life healthier.
American peanut council. Non-Food Uses for Peanuts.
Wood, Robert. Food Allergens in Non-Food Items.
Crash Course on the Most Common Food Allergens
What You Should Know About Peanut Allergies
My Child's School Is Peanut-Free, So What Can I Send for Snacks?
Food Choices for a Soy-Free Diet
Shellfish Allergy? You Need to Avoid These 19 Different Sea Creatures
Tree Nut Allergy Diet Guide
Nut Allergy Guidelines Help Manage Peanut and Tree Nut Allergies
Is Banning Peanuts From Schools for Allergies the Right Way to Go?
Is Coconut a Tree Nut That May Cause an Allergic Reaction?
Is Annatto Safe If You're Allergic to Nuts?
Eating Safely at McDonald's If You Have a Food Allergy
Why People With Food Allergies Should Be Cautious of Cooking Oils
How You Can Help Prevent Food Allergies in Your At-Risk Baby
How to Better Understand Food Allergies
Terrific Holiday Gifts You Can Give to People With Food Allergies
Don't Let These Sources of Peanuts Catch You By Surprise


Here's what happened after her prayer request.
She wanted the figures to be like Frosty the Snowman, who could spring to life at any moment. That's when her vision changed from selling the snowmen to make money to creating something that would make her children laugh.
Motivated by her accomplishments, she pondered whether other families would enjoy her unique snowmen. Later that day, Ulisa traveled to a local shop hopeful the owner would like the snowmen. Of course, the store owner loved Ulisa's crafty creations and ordered 10 more.
The orders kept coming and the Snowman Village Collection was born. What's more, the Rodriguez family ventured to Walt Disney World.
Visit booth #25 to see Ulisa's playful artwork, which also includes seasonal dolls, doorhangers and décor.


Kaiser Chiefs' Nick Hodgson has claimed that guitar music "is at an all-time low".
In an interview with the Birmingham Mail, the drummer said that indie music had experienced a dip in popularity since the band released their debut album, 'Employment', in 2005.
It's a strange time to be in a band. We all know guitar music is at an all-time low.
Kaiser Chiefs released their fourth album 'The Future Is Medieval' earlier this year, for which they wrote 25 songs and allowed fans to choose their own tracklisting.. The band are also set to release a new single that did not appear on the album called 'On The Run' in January, which reportedly takes aim at "rude, cruel people" who use Twitter.
To watch an NME video interview with Kaiser Chiefs, where they explain the concept of 'The Future Is Medieval', scroll down and click below.


Both teams failed to progress from the group which also included Argentina and Belgium.
In the qualifying tournaments, it happened more often.
In Asian 2002 World Cup qualifying, Iran beat its own record (17-0 over the Maldives from 1998 qualifying) by an emphatic win over Guam. However, Oceania couldn't stand back, and Australia improved with a 22-0 over Tonga, and proved conclusively against American Samoa why the OFC do not deserve a full qualifying place: 31-0. American Samoa so far suffered six defeats in double digits in three different qualifying tournaments (2002, 2006 and 2010). In Europe, San Marino also suffered double digit drubbings in three different qualifying tournaments, those for the World Cups in 1994 (0-10 in Norway), 2002 (1-10 in Belgium) and 2010 (0-10 in Poland).
Note that only amateur players were allowed until 1980, and afterwards age restrictions were made, so that not all of the below count as official A-internationals. The Philippines have been a particular welcome source for double digit wins (9 in all) while South Korea and Sweden have both lost and won by 10 goals difference.
Double digits were never reached in the final phase of any European Championship; it happened four times during the qualifying stages. At the first occasion, it was surely no coincidence that Spain needed a win by an eleven-goal margin to reach the 1984 final tournament.
Ireland conceded double digit losses on four occasions in the British Home Championship. Note that all of them happened before the split of the island and at the time, the strongest clubs and players were home in Belfast, in current Northern Ireland.
Double digits are common in the Oceanian Cup for Nations.
This match was abandoned with 10 minutes left to play when Oman walked off contesting the award of a penalty to Libya!
Even this 'record' is now obsolete thanks to American Samoa's participation in the World Cup.
Some trivia: the only clubs to have reached double figures more than once in European competition are Liverpool (3 times), Ajax and Feyenoord (both twice). No fewer than 6 different English and 5 different Dutch clubs have reached double figures at least once, for in total 8 and 7 times, respectively.
The only clubs to have conceded double figures more than once are are APOEL Nicosia (on 3 occasions, all in the CWC), Anorthosis Famagusta, Floriana, KR (Reykjavík), Red Boys Differdange and Reipas Lahti, all twice. No fewer than 5 different Cypriotic clubs (for in total 8 times) and 4 different clubs from Luxembourg and Malta (on 5 occasions in total) have been destroyed in this manner.
The only club to have both reached and conceded double figures in European competition is Anderlecht.
For a full overview of all occasions double digits were reached in the European Cups, check here.
List may not be exhaustive as not all results are known.


Description: Benchmark Construction Inc is a business categorized under general contractors, which is part of the larger category general contractors, single family houses. Benchmark Construction Inc is located at the address in Charlestown, New Hampshire 03603-0000. You can contact by phone (603)863-2772.
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Poor breeders. With their rampant fertility, Baby Björns, and little bundles of adorable obligation, the burdens of parenthood make the activity of concert-going a rare excursion—one that suddenly involves pricey babysitters and a mindful eye on the clock. Of course, you can always pack a tiny Ziploc of Cheerios and take your child with you to a concert, but it doesn't take a Dr. Spock book to realize that kids hate Motörhead—too loud, plus in the eyes of an innocent child, Lemmy's mole is pure evil. And there is only so much Raffi and Baby Loves Disco that any sane parent can stomach.
Thankfully, there is You Who.
Despite the strong indie cred of founders and parents Chris Funk (the Decemberists) and partner Seann McKeel (former booker for venues such as Nocturnal, Acme, and the Wonder Ballroom), You Who is without question a children's show. Set to run monthly at the Kennedy School during daylight hours—it will take a break in the springtime, when the weather warms—this variety show for the shorty set is chockfull of puppets, magic, stories, sing-alongs, and "giant barn owls." But it also has music. Lots of incredible music, especially given the small confines of the space and smaller size of the event's target audience. Funk's own Decemberists kick off the inaugural show this weekend, and future guests include Quasi, Blue Giant, Explode into Colors, and a booking that might deafen an entire generation of future heshers: Red Fang.
"Initially people were like, 'We don't play kids' music,' and we said, 'We don't want you to play kids' music, just play your set,'" Funk explains. Part of the dual foundation of You Who was to establish a family-friendly affair that children will enjoy, yet simultaneously keep their parents entertained as well. Organizing an event that appeals to such varying age groups requires a lot from Funk and McKeel. Evidence of this is the pair of painstakingly assembled giant papier-mâché owl heads that lay decapitated on their dining room floor (not to brag, but it would seem that the Mercury is the preferred publication for use in paper-assembled Tytonidaes).
While many of the scheduled performers are parents themselves, that's not the case with all the bands on the You Who docket: "My niece saw Explode into Colors at the Rock 'n' Roll Camp for Girls and she was the one who said, 'Oh my god, you have to get them,'" explains McKeel. Another hurdle came in trying to attract families, first and foremost, and not just fans of the performing musicians—not to say that the Youth and Beauty Brigade that follows the Decemberists wouldn't enjoy a nice puppet show during the afternoon. You Who's pricing structure charges adults without children $5 more to attend, not exactly punishing them, but just a reminder that they aren't necessarily the intended audience. As Funk puts it, "The first hour is variety entertainment and very much tailored to children. I think people would be let down if they paid to see this concert and they thought it was something else." McKeel adds, "We didn't want a bunch of 25-year-old indie rockers not getting the comedy... which is animal impressions."


text:
Cameron Diaz leads a knockout cast in this irreverent comedy about love, lust and the laws of karma. New York attorney Carly Whitten (Diaz) is nobody's fool. So when she accidentally discovers that her too-good-to-be-true boyfriend Mark (Nikolaj Coster-Waldau) is married, she's less than thrilled. Not only that, she and Mark's wife Kate (Leslie Mann), learn about yet another mistress (Kate Upton)! Before long, however, the betrayed beauties have become unlikely pals who've decided to teach their three-timing man a lesson. The more the trio learns about Mark, the worse he seems, and the more fun they have without him!
Starring Cameron Diaz, Leslie Mann, Kate Upton
Director Nick Cassavetes
Carly Whitten
Mark King
Taylor Kinney
Kenneth Maharaj
Julie Yorn
Donald J. Lee Jr.
Chuck Pacheco
Melissa Stack
LBI Productions
© 2014 Twentieth Century Fox Film Corporation. All rights reserved.
English (United States) (AAC, Dolby 5.1), French (France) (AAC)


After 25 years in the industry as head of Building Surveying at a major multi-disciplinary partnership, Building Surveying & Project Management was established by David Golland in 2003. BSPM focusses on providing clients with efficient, reliable and professional advice with a straightforward approach.
BSPM provides a full range of Building Surveying and Project Management services to corporate, commercial and private clients over a wide geographical area . Based in Basingstoke, the majority of our work is in Southern England but instructions have ranged from Penzance to Aberdeen and all points between.