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Article by Ann Oppenhimer
After 16 years, it's time to take stock of the Folk Art Society of America's major events and accomplishments. We have received many requests for this information, making us realize that perhaps members who have not been a part of the organization from its inception may not be aware of what other members often take for granted. Therefore, we are including in the Web site a new article, "16 Years: A History of the Folk Art Society," illustrated with old photographs from FASA's files. It's part of our ongoing historical documentation — making lists for the record books, if you will. The striking cover of the Spring Folk Art Messenger recapitulates the color covers from the past five years.
An event that has caused a personal stock-taking has been the exhibition of our own collection, Point of View: American Folk Art from the William and Ann Oppenhimer Collection, which originated at the University of Richmond's March Art Gallery on October 12, 2001. The exhibition had been scheduled to finish its scheduled tour of six venues on April 13, after traveling to Longwood University in Farmville, Va., Orlando's City Hall Terrace Gallery in Florida; The Art Museum of Western Virginia in Roanoke, Va.; Sweet Briar College in Amherst, Va.; and the Contemporary Art Center in Virginia Beach. My husband and I attended each opening reception, and I gave a slide lecture or gallery talk at least once in each museum. At every stop, the directors, curators, registrars, educational directors and security personnel were most professional, cordial and enthusiastic. We enjoyed the receptions, the lectures, the newspaper and magazine articles — and we appreciated this once-in-a-lifetime experience. Now, there has been a new development: We have received word that several additional showings of the exhibition have been requested, and the art works will continue their journey through at least 2004.
Richard Waller, director of the University of Richmond Museums, selected the artworks for the exhibition, first by looking at photographs and then by looking at the objects scattered throughout our home. He asked us to make a list and take pictures of the pieces we felt should be in the show, saying he would study these and make a tentative list. When we met to make the final decision, he told us that he had about 60 pieces on his list. We had 140 pieces on our list, and we knew we had a problem. I said, "Richard, we have more that 100 pieces in the living room." Richard quickly replied, "But we don't want the exhibit to look like your living room!"
Folk art collectors can understand the problem. We think more is more, and sometimes a collection can get out of hand. We did compromise on 86 works, approximately half sculpture and half two-dimensional paintings, drawings and serigraphs. Four works were deemed too fragile to travel and were seen only in Richmond.
It's a revealing experience to see your collection through the eyes of others. Certain objects looked much better in the well-lit galleries than they did mixed with the furniture and trappings of daily life. Friends who came to the exhibition often remarked, "Where was that? — I never saw that piece before," about an object that must have been visually lost in our living room.
After the exhibition completes its tour, it will be disassembled, put into the specially built crates and returned to us. We'll be glad to see certain favorites that we really have missed. Other pieces we found we could easily live without. Even in the selection of 80-odd pieces, there is a hierarchy of quality that is obvious. This realization brings up another question: What will happen to our collection when we can no longer look after it? That's a question that even minor collectors like us will have to face some day.
Several remarkable collections have been dispersed in the past several years. The Michael and Julie Hall Collection was purchased by the Milwaukee Art Museum; the Herbert Hemphill Collection went to the Smithsonian American Art Museum by gift and purchase; the Rosenak Collection went to the SAAM by gift/purchase; a part of the Marshall Hahn Collection was given to the High Museum of Art in Atlanta, and the rest was auctioned by the museum. The preservation of these collections in museums has enriched us all. Other collections have been dispersed by auction. Warren and Sylvia Lowe's collection was auctioned at Slotin Auctions, as was Myron and Cecille Shure's; a portion of Robert Greenberg's collection was auctioned at Christie's in January. The break-up of these collections is interesting to collectors for its effect on the folk art marketplace and for the recirculation of pieces into other private and public collections.
As for our collection — which is not remarkable and is not intended to be compared to the above-named ones — the experience of acquiring the art from the artists has brought us many happy times and memories. We hope that our work with the Folk Art Messenger and the Folk Art Society has helped to repay our debt in some small way to the remarkable people who made the art.
Ann F. Oppenhimer, President
Folk Art Society of America
ANN OPPENHIMER is the Executive Director of the Folk Art Society of America
As seen in the Folk Art Messenger:


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Some days nothing goes right….
London, England A motorist tried to commit suicide by driving over a cliff – only to be prosecuted for drink driving.
John Corner was suffering from depression when he headed to the rockface with lots of alcohol. He parked close to the edge, had a drink to summon up courage and drove straight for the precipice. But his car stopped just inches from disaster after hitting a fence. He was found by police close to the scene and was arrested – for drunk driving the short distance from where he had stopped to the edge of the cliff…
Mr. Corner, believed to be from Southend-on-Sea, Essex, won his appeal on the grounds he was not a danger to other road users while driving towards the cliff's edge.
Apparently, police in England have about the same degree of common sense and compassion as their brethren in America.
(Thanks to Richard Diamond.)
The post Attempted Suicide Convicted of DUI appeared first on Law Offices of Taylor and Taylor - DUI Central.

subset: commoncrawl


text: A negative control should also be included when performing siRNA experiments to eliminate the possibility of nonspecific silencing effects. For this purpose, Gene Link provides a siRNA sequence that has been shown to have no effect on gene silencing. The negative control siRNA is also available labeled with fluorescein, which allows transfection efficiency to be tracked by fluorescent microscopy.


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'Lord Of The Meows' Personalized Tumbler
Digitally Illustrated By Hand
Enjoy your favorite beverage from an epic personalized masterpiece featuring your cat (or any pet!) with our personalized Viking Tumblers!
Our premium 7" stainless steel tumblers are double wall vacuum sealed with copper lining and will keep your beverages warm for 5-6 hours or cold for 24 hours!
The Process: We Make It Simple
- Pick your desired tumbler color (Stainless, Black, Mint, Copper, or White)
- Upload a photo of your pet using our easy upload button
- Place your order
- Leave the rest to us!
- Proudly made in the USA and dispatched worldwide within 2-5 business days.
• Please upload a clear close-up frontward facing photo of your pet at eye level and appropriate light (natural outdoor light works better than flash, try to avoid bad lighting and blurry photos).
• Make sure your pet's ears are within the photo frame and not cut off!
• Please do not upload a photo of a photo or a screenshot of a photo, uploading an actual photo will have a higher resolution.
After uploading your first photo, you can upload more by selecting on the left hand side menu of the uploader where you want to upload the file from: Local Files (most common), camera, Facebook, etc.
Where are tumblers shipped from/to?
We proudly produce and ship our tumblers from the USA. We ship worldwide!
How long does production take?
Current production time is an estimated 2-3 business days.
How long does transit take on average?
USA Estimates: 3-5 business days
Canada/UK/Australia/Europe: 10-21 business days.
Rest of the world: 15-30 business days.


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With rising purchasing power and changing consumer lifestyles, the global dairy market is growing. A health-conscious generation has a strong belief in milk's benefits, and the demand for dairy products is anticipated to significantly increase in countries like India and China.
Given our 120 years of experience in the dairy industry and our deep knowledge and understanding of dairy technology, we are well equipped to help you give milk and other dairy products the desired properties required for different finished products.
We offer a complete portfolio of dairy processing and packaging solutions and can supply everything from a single valve to a complete green field factory.
We reach dairies around the globe, applying our thorough technological know-how to help you to seize market opportunities and extend product ranges. Our annual report, the Tetra Index, is designed to help dairy producers identify new opportunities for growth.
Get insights into processing technology and the entire chain from cow to consumer – from pasteurization, homogenization and UHT treatment, to filtration, automation, service systems, waste water treatment and many other aspects of modern dairy processing with the Dairy Processing handbook now also available online.


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Iconic $110 Million Hilton Nairobi Upper Hill Marks Hilton Hotels & Resorts' 50th Property.
The hotel is set to open in 2020 and joins 50 Hilton Hotels & Resorts properties trading or under development in 17 countries across Africa.
"In recent years Upper Hill has grown to become a hub for international businesses and organisations, with a number of embassies and organisations setting up their regional offices in the district, including Cisco Systems, World Bank and the IMF," said Patrick Fitzgibbon, senior vice president, development, EMEA, Hilton Worldwide. "The striking new-build property will pierce the skyline of Upper Hill and will be well placed to meet this growing demand in one of Nairobi's most exciting and colourful areas."
Kenya is one of Africa's fastest growing economies with strong growth in agricultural, tourism, construction and telecommunication sectors. The country's diversifying economy means it is a popular destination, busy with leisure and business travellers.
Mr Mahat Noor, Project Director of Jabavu Village Ltd, said, "Hilton Nairobi Upper Hill is our first project with Hilton and we are tremendously excited to be collaborating with them on this spectacular development. Hilton Nairobi Upper Hill and the larger mixed-use development, which will include a residential, retail and entertainment complex, as well as an adjacent office tower, will be Africa's tallest building, standing at 330m."
Co-developed by Jabavu Village and White Lotus Projects, Hilton Nairobi Upper Hill will comprise of an Executive Lounge and five food and beverage outlets, including a relaxing poolside bar, speciality smokehouse and grill restaurant, lobby dining area with landscaped deck and a boutique rooftop bar with unbeatable vista views of the Nairobi skyline on the 43rd level.
Business travellers will have a wide choice of professional facilities to choose from including a ballroom and meeting rooms of approximately 1400sqm. Guests will also have access to an outdoor pool and fitness and spa centres.
Hilton is set to double its presence in Africa in the next three to five years and is focused on further development prospects all over the continent, entering new countries but also growing in areas with an existing Hilton presence.
Hilton Nairobi Upper Hill joins one other Hilton Worldwide hotel under development in Kenya. Hilton Garden Inn Jomo Kenyatta International Airport will be situated just 2km from the capital's airport and is set to open next year. Hilton Nairobi Upper Hill will be situated 16km from Jomo Kenyatta International Airport, on Upper Hill Road, Upper Hill, Nairobi, Kenya.


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Dec 142017
Need help with maintaining and updating your ecommerce / online store? You should establish a relationship with ecommerce specialists to help you keep your site updated, secure, protected and to add new functions and features. Here is one company that can help you with your online store maintenance in the New York, NY, USA and pretty much everywhere else.


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Posting a New Topic |
When you go to a forum you are interested in and you wish to create a new topic (or thread), simply choose the button at the top and bottom of the forums entitled "New topic". Please take note that you may not have permission to post a new topic in every forum as your administrator may have restricted posting in that forum to staff or archived the forum entirely. |


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A U.S. Air Force F-35 Lightning II, F-16 Fightning Falcon and two P-51 Mustangs fly in formation during the 2018 Heritage Flight Training and Cerification Course at Davis-Monthan Air Force Base, Ariz., March 3, 2018. During the course, aircrews practice ground and flight training to enable civilian pilots of historic military aircraft and U.S. Air Force pilots of current fighter aircraft to fly safely in formations together. (U.S. Air Force photo by Senior Airman Mya M. Crosby)
No camera details available.
This photograph is considered public domain and has been cleared for release. If you would like to republish please give the photographer appropriate credit. Further, any commercial or non-commercial use of this photograph or any other DoD image must be made in compliance with guidance found at https://www.dimoc.mil/resources/limitations, which pertains to intellectual property restrictions (e.g., copyright and trademark, including the use of official emblems, insignia, names and slogans), warnings regarding use of images of identifiable personnel, appearance of endorsement, and related matters.


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Last night I was going through some old pictures of Chicky Baby. Old in comparison to her time on this earth so far, that is, which is to say ones taken maybe 300 days ago. She's beginning to look so much more like a little kid than the wee, snuggly baby I used to rock to sleep...
(who am I kidding, she never went for that whole rocking-to-sleep thing. I had a better chance of teaching her the rumba than getting her to sleep before the age of five months. She was a stubborn little thing. Anyhooo.)
... that I'm beginning to forget the look of her sweet little baby form and her pink baby lips and her soft, downy baby head (which we're seeing a lot more of these days - pictures tomorrow, I promise.). I guess it put me into a bit of a melancholy funk.
Melancholy Funk. Wow. That's a great name for a band. I can see this band covering Nina Simone songs and maybe some Sly and the Family Stone. After this year's Grammys you just know Sly Stone needs a decent gig. Does anyone know if Bootsy Collins is available? To pull off the whole melancholy thing he'd have to leave the Bedazzler at home, so he probably wouldn't go for it.
Uh, where was I?
Oh, yeah. Melancholy funk.
The last couple of days I've gone back and forth between feeling like I'm really in serious love with this new toddler stage and praying to any higher power who will listen to please, for all that is good or unholy, please give me my sweet baby back.
I want my baby back, baby back, baby back.
So I thought I would post one of my favorite pictures from Chicky's infant days. This one never fails to make me smile. If you're having a melancholy funky day I hope it will make you smile as well.
New at Dog Gone Blog: Kong stuffers (no, not things you'd put in the Christmas stocking of an extra large ape with an attitude) and dog tag silencers. Good times, good times.
Bitacle Steals Content!
If you're not reading this on www.chickychickybaby.blogspot.com or a feed authorized by the author then you are viewing stolen content. Please read this on the site it was legally published on and not on a splog like Bitacle who steals other people's work for their financial gain.


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Gabriel (de Vylder) of Komana
His Excellency the Most Reverend Archbishop Gabriel (de Vylder) of Komana was the primate and exarch of the Patriarchal Exarchate for Orthodox Parishes of Russian Tradition in Western Europe, a diocese under the jurisdiction of the Ecumenical Patriarchate. He served from 2003 to 2013 before his retirement.
Guido de Vylder was born in June 13, 1946 in Lokeren, near Ghent (Belgium), into a Flemish Catholic family. He received technical training as he was to succeed his father as head of the family business. After serving his military obligation in 1966, he entered the Institute for Delayed Vocations in Kortrijk. In 1970, he studied philosophy and theology at the Seminary of Ghent before changing his area of studies to morale and religious studies at Catholic University of Louvain from which he graduated in 1976.
During this time he became acquainted with the Orthodox Christian parishes in Belgium and the Netherlands which led him to refuse ordination to minor orders in the Roman Catholic Church. In January 1974, he was received into the communion of the Orthodox Church at the Parish of St. Andrew in Ghent.
On October 5, 1975, he was ordained a celibate deacon by Archbishop Georges (Tarassoff) of Syracuse in the Crypt of the Holy Trinity Cathedral of St. Alexander Nevsky in Paris. On June 27, 1976, he was ordained priest also by Abp. Georges in Holy Trinity Cathedral.
In 1977, he was assigned as first priest of the parish of Saint Jean-Chrysostome in Maastricht, Netherlands. During this time he also participates in the establishment of parishes in Deventer, Breda, and Antwerp. On March 9, 1985, he was elevated to archpriest. On December 12, 1992, he was appointed rector of the parish of St. Alexander Nevsky in Liege, Belgium by Abp. Georges (Wagner).
On May 11, 1994, he took his monastic vows, with the name Gabriel, before Abp. Sergius of Eucarpie, at St. Sergius in Paris. On December 10, 1995, he was elevated to an abbot and on December 20, 1998 to archimandrite. On December 17, 1998, he was appointed rector of the parish of Maastricht, while retaining his duties in Liege.
In January 2001, the Holy Synod of the Ecumenical Patriarchate elected Fr. Guido auxiliary bishop of the Exarchate of Orthodox Parishes of Russian Origin in Western Europe with the title "Bishop of Komana". Consecrated bishop on June 24, 2001, he was given responsibility for the parishes in northern France, Belgium, the Netherlands, and Germany.
In December 2002, Abp. Sergius of Eucarpie became ill and assigned the task of administering the archdiocese to Bp. Gabriel. Following the death of Abp. Sergius on January 22, 2003, the Synod of the Archdiocese elected Bp. Gabriel Locum Tenens of the archdiocese. The clergy and laity of the General Assembly of the archdiocese, meeting in Paris on May 1, 2003, elected Bp. Gabriel to lead the archdiocese. His election was confirmed with the rank of Archbishop by Holy Synod of the Ecumenical Patriarchate on May 3, 2003. His enthronement took place in the Cathedral of St. Alexander Nevsky in Paris on June 1, 2004, attended by clergy and laity of Paris, the Paris region, the provinces, Belgium, the Netherlands, and Germany.
Abp. Gabriel was a member of the Assembly of Orthodox Bishops of France. He was also the rector of the Theological Institute of St. Sergius in Paris.
On January 8, 2013, Abp. Gabriel formally requested retirement of the Patriarch of Constantinople for health reasons. On January 15, Metr. Emmanuel, Greek Metropolitan of France, was appointed locum tenens pending the election of a new ruling bishop in May 1913. Abp. Gabriel retired to the city of Maastricht in The Netherlands.
Gabriel (de Vylder) of Komana | ||
Preceded by: Sergius (Konovaloff) |
Archbishop of the Russian Orthodox Exarchate in Western Europe 2003-2013 |
Succeeded by: — |
External links
- Official biography on the page of the Orthodox Church of Belgium (French)
- L'Archevêque : Mgr Gabriel, exarque du Patriarche œcuménique (in French)
- Hierarchical entry in the database of the Orthodox Research Institute
Categories > People > Clergy > Bishops
Categories > People > Clergy > Bishops > Bishops by century > 21st-century bishops
Categories > People > Clergy > Bishops > Bishops by city > Bishops of Komana
Categories > People > Clergy > Bishops > Bishops by city > Bishops of Paris
Categories > People > Converts to Orthodox Christianity
Categories > People > Converts to Orthodox Christianity
Categories > People > Converts to Orthodox Christianity from Roman Catholicism


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The statistics are sobering. The typical American diet far exceeds the daily recommended intake levels in calories from sugars and solid fats, sodium, refined grains, and saturated fat. It is also lacking in the recommended amounts of fruits, vegetables, dairy, whole grains, and oils. The result is obesity and experts project that by 2030, in the United States alone, half of all adults will be obese.
That's when people start dieting – and that is what gets them into trouble.
Diet vs. Lifestyle Change
Bottom line, diets are temporary. There are some serious consequences that can come from dieting, especially fad or crash diets. The effects of these types of diets can also seriously impact your chiropractic care, hindering your progress.
Also, because diets are temporary, once you return to your regular eating habits the weight usually comes back.
A lifestyle change is a far better choice. It involves making smart, healthy eating choices – choices that you maintain for the rest of your life. This also impacts your chiropractic care by strengthening your body and keeping it healthy so that it is in an optimal state for healing and responds well to treatment.
Types of Diets
There are all sorts of diets out there. Some are blatantly unhealthy but others are sneaky. They come with claims of being healthy, of being created or endorsed by doctors, or include tons of vitamin supplements but very limited food intake. It is important to be able to spot these destructive fad diets so you don't get suckered into their hype.
Some of the most common types of fad diets include high protein, low or no carb, liquid, cabbage, grapefruit, broth or juice, and food combining. Some of these can cause serious health problems including vital organ damage. Others can cause vitamin deficiencies and dehydration. None of them can (or should) be maintained over a long period of time, much less the rest of your life.
The Dangers of Diets
Unhealthy dieting can come with some pretty scary dangers. Because they typically omit key foods or food groups your body can become imbalanced. Some of the dangers of dieting include dehydration, fatigue, weakness, vitamin and mineral deficiency, headaches, nausea, diarrhea, constipation, mental fogginess, loss of muscle mass, organ damage, and even heart attack and stroke.
One popular diet restricts carbs, often cutting them out completely. This includes all whole grains (which have vital minerals and fiber) as well as many fruits and vegetables. The result is a diet that is mostly protein and fat.
While the dieter may lose some weight on this plan, it is at a great cost. The extremely high intake of protein which exceeds the levels that the body should have can cause liver and kidney failure. The omission of vital grains, fruits, and vegetables can lead to serious vitamin deficiencies while the increased fat intake can lead to heart attack and stroke.
If a diet eliminates any of the key foods (lean meats, whole grains, fruits, and vegetables), it advocates losing more than 2 or 3 pounds a week, or it restricts caloric intake to less than 1,200 calories a day it is potentially unhealthy and should only be done 1) under a doctor's close supervision, and 2) on a very temporary basis.
Healthy Eating is a Lifestyle
When you make the life changing commitment to adopt a healthy eating lifestyle you open yourself up to a world of better health, more energy, and better focus. Your body will heal faster and you will feel better.
A diet of fresh fruits and vegetables, lean meats, fresh fish, and whole grains, along with lots of water should become a way of life. It is far healthier than the temporary diets that are out there and more effective too.
If you or a loved one need additional dietary guidance, give us a call. Our Doctor of Chiropractic is here to help!
This article is copyrighted by Blogging Chiros LLC for its Doctor of Chiropractic members and may not be copied or duplicated in any manner including printed or electronic media, regardless of whether for a fee or gratis without the prior written permission of Blogging Chiros, LLC.


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27inch Android Display - Non Touch
Product Code: EL-2703AIO-OS9.0-RK3399
30-day money-back guarantee
Free Shipping in U.S.
Buy now, get in 2 days
Android Display
Our Android Displays are commercial models, specially designed and to use in a retail environment, online digital signage screens, info touch kiosk, etcetera.
The Android has a standard some programm apps installed, like a browser, google play store, explorer, and some extra apps.
You can install your own application on it. For instance a digital signage app or kiosk web app, webstore, etcetera.
We can also provide and help you with some retail app solutions, to help you to start your project. Find more about these apps at the software section.
These Android Displays have the following features:
- - Touchscreen & Non-Touchscreen
- - ROOTED ANDROID 9.0 software version
- WIFI network - - LAN (RJ45) input socket for a cable network connection (not for all models)
- - 3G-4G connection via USB SIM dongle (optional, not included)
This desk-model shape is available in: 10.1 / 13.3 / 14 / 15.6 / 18.5 / 21.5 / 24 / 27 / 32 / 43 / 55 inch sizes.
How does it work?
Watch this video to have an more detailed explanation how these Android screens work.
List of Features
easy setup and plug and play!
Auto Start when plug in the power adapter
Rooted Android 9.0 / Chip RK3399 / RAM 2GB-IM 16GB / CPU Quad core cortex A53, 2.0G
Non Touch
27" LCD panel 1920x1080 pixels (16:9 ratio)
Internal HD videoplayer 1080P
WIFI, Bluetooth, optional LAN and 3G
SD cardreader and 1x USB portal
Internal Speakers
3.5mm Jack Output
Thin Closed Frame Plastic Housing
Color housing standard Black, Optional white.
12V Power adapter with 3 meter long cable
24/7 usage
Timer Clock Function (optional app)
can be used in many places
Digital Signage Display
Built-in ShopDisplays
Advertisement Display
Shelf-edge Display
Plug in the power adapter, and immediately the Android display will turn on (no need to push a ON-OFF button).
You can hide the top and bottom bar in the Settings menu.
Install your software easily and lets play!
- with or without internal battery
- LAN converter box, to connect to the portal at the backside.
see SPECIFICATIONS TAB or download the specification sheet in the DOWNLOAD TAB, above.
Screen size |
27inch |
Screen type |
Non-Touchscreen |
LCD Panel Type |
LCD Panel resolution |
1920*1080 |
Ratio |
16:9 |
Optional Features |
Software Systems for Digital Signage & Kiosks , 3G Network via USB-SimCard Dongle |
Operation System |
Dual Core A72 , Quad Core A53 , Rooted , Android 9.0 - RockChip RK3399 |
Interface - Connection portals |
LAN , HDMI OUT , SD Cardreader , USB Portal , Mini USB Portal , 3.5mm Jack , Power Input DC 12V/4A |
Resolution Internal VideoPlayer |
1920*1080 |
Housing type |
Closed Plastic Frame |
Start-Up |
AutoStart by plug-in the power-adapter |
Usage |
24/7 |
Network options |
Wifi , LAN/WLAN , Bluetooth 4.0 , Mobile Network (3G-4G) - Optional by USB SIM Dongle |
Speakers |
2x 3W |
Mounting options |
VESA 100x100mm - screwholes 4mm |
Memory |
RAM 2GB - Internal Memory: 16GB |
Camera |
2.0MP front camera |
PowerAdapter |


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In the spring of 2012 my floor level valuation methodology was illustrated in a great piece in New York Magazine by Jhoanna Robledo called "What Price Height and Light?. The graphic and accompanying descriptions provide incredible clarity to a fairly convoluted subject.
In the flurry of transitioning content to our new site over the past few months, I remember the actual moment when I deleted the original post for this topic by mistake and thought, "wow this is annoying but I can always go the Wayback Machine." However, today someone asked me about the graphic and I couldn't find my prior post on the Wayback Machine (but I found a bunch of cool stuff) so I am reposting this piece. I really LOVE the graphic that New York Magazine came up with.
The graphic is fairly self-explanatory.


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Need a large quantity of ideas in a short amount of time? Brain writing might be the ideal solution. Gather up a group of thinkers and watch the ideas pour forth.
Brain writing is a brainstorming solution that uses the power of a group to generate a large quantity of ideas. Here's one way to get started: simply identify a moderator, gather six participants with paper and pens/pencils and follow these simple instructions:
Gather your participants together in a room, along with your moderator.
Identify the topic you want to solve for and have each participant jot down their thoughts/solutions on a Post-it® Note.
After 5 minutes have passed, hand your thoughts over to one of the other participants. Someone will hand you his/her thoughts as well.
Read through the ideas you received and use them as a starting point to generate an additional three ideas inside of five minutes.
Voila! After six rounds/30 minutes, your group will have generated 108 ideas...and will probably need a cold pitcher of water.


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Calibration Overview
This document provides an overview on how calibrations will be performed with EOVSA, and what the implications are for monitor, control, pipeline and analysis software. Here is a summary table (Table 1), followed by more detailed discussions.
Table 1: Summary of EOVSA Calibrations† | |||||||
Calibration Type | Calibration Item | When Calibrated | Reference Source | Analysis Type | Solution Type | Applied by | Criticality |
Pointing Calibration | Antenna pointing errors | Occasional | Sun, sat, brgt cosmic src |
Offline | Per ant | Control System | High |
System Gain Calibration | Attenuator gain variation | Occasional | ND, Sun | Realtime | Per ant, poln | DPP Stage-2 | High |
Total power response | Occasional | ND, Sun | Offline | Per ant, poln | DPP Stage-2 | High | |
System non-linearity | Occasional | ND, Sun? | Offline | Per ant, poln | DPP Stage-2 | Normal | |
Spectral similarity | Precalculated | Sat? | Offline | Per ant, poln? | DPP Stage-2 | High? | |
Delay Calibration | Fine delay | Precalculated | N/A | Offline | Per ant, poln, IF | Correlator | High |
Delay center | Occasional | Sat, Brgt cosmic src | Offline | Per ant, poln | Correlator | High | |
Residual delay | Daily-weekly | Brgt cosmic src | Pipeline | Per ant, poln, IF | Pipeline | High | |
Bandpass calibration | System bandpass pattern | Daily-weekly | Brgt cosmic src | Pipeline | Per ant, poln, chan | Pipeline | High |
Reference Gain Calibration | System complex gain w.r.t. point source |
Daily-weekly | Brgt cosmic src | Pipeline | Per ant, poln, IF | Pipeline | High |
Daily Gain Calibration | Time-dependent complex gain w.r.t. point source |
~Hourly | cosmic src near Sun |
Pipeline | Per ant, poln, IF | Pipeline | High |
Polarization calibration | Differential feed rotation | Occasional | Brgt cosmic src | Realtime | Per ant | Correlator | High |
D-term and R-L angle | Occasional | Brgt cosmic src, sat? | Offline | Per ant | Correlator | Normal | |
Baseline correction | Antenna position error | Occasional | Multiple cosmic srcs, sats | Offline | Per ant | Correlator | High |
†Modified from Gordon Hurford's list of calibrations (v2010-Nov-16) -- BC, 2016-Sep-24
Pointing Calibration
Pointing calibration is antenna-based (has to be done separately for each antenna), and entails an initial determination of pointing errors to create a set of pointing correction coefficients, followed by periodic checks of pointing and possible updating of coefficients as necessary. For KSRBL, initial pointing determination was done optically by mounting an 80 mm optical telescope and small CCD camera on the dish, and doing a single 1-night set of measurements of star fields. This provided excellent determination of correction coefficients around the sky, leaving a simple az-el offset to be determined by solar pointing (because the optical and radio axes were not guaranteed to be parallel). The analysis of the set of optical measurements was complicated, but could and should be automated. However, the assumption is that this only has to be done once during initial commissioning of an antenna. The determination of the az-el offset is then accomplished by a single determination of the solar radio disk position. Note that there will be differences in the radio beam position vs. frequency, so any determination of solar disk position will vary with frequency and must be optimized in some way, probably weighted to the highest frequencies, which have the smaller beam.
Once the pointing coefficients and offset are determined, they can be optimized and updated periodically by a pointing calibration, and it is that calibration that is further described here. There are several options: (1) determination of the offsets of the solar radio disk (requires the Sun, and may be skewed by active regions—also limited to a single declination), (2) determination of the position of other bright objects such as satellites (valid only at discrete frequencies where such satellites are broadcasting), and (3) interferometric pointing on cosmic sources or planets using one or both of the 27-m dishes. Each of these has merits, and all will likely be implemented.
Solar Pointing Calibration
This is based primarily on the scheme developed for KSRBL (Dou et al. 2009, PASP, 121, 512). The pointing offsets for all antennas can be determined simultaneously, and as a function of frequency, by offsetting each antenna in a cross pattern and measuring the total power spectrum. This provides multiple useful parameters: (i) frequency-dependent pointing offsets, which can be surprisingly large, and are necessary for primary beam corrections to all interferometer amplitudes, (ii) direct measurement of the primary beam size and shape, and (iii) a check on overall total power gain calibration relative to that determined interferometrically on cosmic sources.
This type of pointing can be done quickly (in less than 20 minutes for KSRBL, possibly much faster if we can devise an antenna control scheme that provides accurate scans) and may even be done daily. It does take time from solar observing. Note that an alternative is to take an antenna out of the array and do the pointing scan in a separate subarray while the rest of the array continues observing. A special antenna control sequence (trajectory) would be implemented, along with standard analysis software independent of the pipeline (since it is only total power). The analysis could be part of the monitor/control system, or offline, depending on how regularly it is done and how integral the results are to the overall calibration. This is TBD.
Satellite Pointing Calibration
It is possible to track satellites across the sky and apply offsets relative to the tracked position in order to do total power pointing measurements. This unfortunately can be done only at a few spot frequencies, and may be too limiting to be useful. Communication satellites are good for this purpose, but are largely geostationary and often too close together, which severely limits their usefulness. Navigation satellites such as GPS have excellent sky coverage, but GPS operates only at very low frequencies where the primary beam is large, so it remains to be seen whether pointing measurements at such low frequencies can be done precisely enough to be useful. There may be a few other satellites that broadcast at higher frequencies. Given the limited resources, it seems wise to defer consideration of this type of calibration unless and until it becomes clear that it is actually needed.
Interferometric Pointing Calibration
Should it be necessary to obtain radio-measured pointing coefficients over the whole sky, only interferometric calibration can work given the lack of sufficiently bright sources for total power calibration. Interferometric calibration will require at least one baseline with a 27-m antenna and a 2-m antenna, and is done by pointing the 27-m antenna at a strong cosmic or planetary source and then pointing the 2-m antenna is a cross pattern similar to the technique used in solar pointing calibration. The phase center tracks the source, and the position of the peak of the interferometer amplitude will provide the pointing offsets. In contrast with solar pointing, which can be done with individual frequency sub-channels, it is likely that the sensitivity of the measurement will limit the measurement to integrated 500 MHz bands. Thus, interferometric calibration will not be very useful for frequency-dependent pointing measurements like the solar pointing, but will be useful for determining some average offset as a function of position over the sky, which is all that is needed for determining the pointing coefficients. This has the advantages of (i) not requiring the Sun, so does not impact time on the Sun, and (ii) obtains pointing offsets over the entire sky rather than being limited to a single declination. Because it uses interferometric results, it will have to come through the correlator and DPP. The analysis would have to be part of the pipeline, or else be done offline.
Table 2: Summary of Pointing Calibration Options | ||||||
Calibration Type | Impacts Solar Observing? | Products | Uses | Control Requirements | Analysis Requirements | Priority |
Solar pointing | Yes | (i) Pointing offset spectrum (ii) Primary beam size (iii) Solar total power spectrum |
(i) Determine pointing corrections at single declination; also amplitude gain coefficients (ii) Amplitude gain (iii) Solar flux calibration |
Antenna trajectory control | Total power analysis could be offline | Essential - best way to get total power gain vs. frequency |
Satellite pointing | No | Pointing offset at a few frequencies | All sky pointing Correction | Antenna trajectory control | Total power analysis in small range of relevant frequencies | Defer |
Interferometric pointing | No | Pointing offset spectrum at 500 MHz resolution | All sky pointing correction | Antenna trajectory control | Pipeline or offline interferometry | Desirable/Needed |
System Gain Calibration (incomplete)
This refers to the periodic (daily?) determination of several system parameters affecting the total power gain: (i) Attenuator nominal values, (ii) noise diode increment, (iii) total power non-linearity. These are simultaneously determined by cycling through all attenuator settings, once with noise diode off and again with noise diode on, and recording the total power level (separately for each antenna). The exact scheme to be followed depends on the system design. This figure summarizes all the gain control "knobs" in the analogue and digital system.
This attenuation scheme uses the Day/Night calibrator as a single setting, while the others are variable in 1 dB steps. The Day/Night attenuator difference of 17 dB is probably too much. The solar variation attenuator in the front end applies to the entire 1-18 GHz RF band, and sets the overall power level to keep the optical link in its linear range. Note that strong fluctuations in a narrow band (e.g. spike bursts) will have less effect when integrated over the entire RF band, so changes to this attenuator should normally be slow and steady during solar bursts. In the back end, the attenuation is applied in the IF (650-1150 MHz) chain. The first attenuator is for leveling the receiver in the absence of bursts. Once leveled, the settings for each receiver will vary with IF band, but will be fixed in time. The second attenuator is for maintaining the output level during solar bursts, and it is this attenuator that will need to be controlled on a relatively fast timescale. Each attenuator will need to have each of its steps calibrated. The two back end attenuators will be in a single integrated assembly, and are best measured offline using test equipment. Assuming adequate temperature control, they should be stable, and changes would indicate a failure of the assembly. Thus, a maintenance test can be conducted periodically to check their values, but it should not be necessary to have a daily gain calibration procedure that checks every IF attenuation setting.
We therefore assume that only the two front-end attenuators will be checked, through a gain calibration procedure, on a regular basis. Will it be necessary to do the procedure in different IF bands, to check for frequency-dependent variations in attenuation? If such variations can be characterized once in the lab, it may be possible to do the measurement in a single, RFI-free band chosen as the standard one for the measurement.
Observational Procedure
In the current OVSA gain calibration scheme, the antennas are pointed at blank sky and the RF attenuation is switched to each setting in turn, switching the noise diode on and off during the measurement. Each IF band is also measured, but the results are combined to give a single attenuation value for each setting, i.e. no frequency-dependent variations are considered. Note that for the current OVSA it is possible to insert so much attenuation (55 dB) that the front-end signal can be assumed to be zero, allowing for receiver offsets to be determined. The maximum attenuation in Fig. 2 is only 36 dB (less if the Day/Night attenuator is reduced).
Delay Center Calibration
Delay center calibration involves sweeping the delays around their nominal value while observing a strong source interferometrically, in order to determine the optimum setting for the delays. For OVSA, the optimum delay is determined by a peak in the amplitude on a particular baseline, whereas for EOVSA it will more likely be done by flattening the phase response across the bandpass. For EOVSA, the current plan is to implement delays in the correlator, so sweeping the delays would be implemented there.
Delay Tracking
It is useful to look at some issues related to delay tracking (ref. the A. R. Thompson FASR memo, "FASR_Delay_Fringe_Phsw.pdf"). For the currently considered design, the ADCs will operate at a clock rate of 1200 MHz, or sample time τs = 0.833 ns, so coarse delays of that step-size will be trivial to implement using a shift register. In tracking the delay, we would change the delay when the delay error is, say, +1/2 τs, making it then -1/2 τs, so this is the maximum delay error. It is interesting that the bandwidth and the sample time are not independent, but rather obey the Nyquist criterion 1/τs = 2Δν, so that Δντs = 1/2. Assuming that the IF band ranges from 0 to Δν (600 MHz in our case) the maximum phase slope across the band, for delay error τ, is Δφ = 2πτΔν = π/2, where τ=1/2τs was used. Therefore, the highest IF frequency channel's phase will vary linearly with time between -π/2 and +π/2. The rate of delay obeys the equation
where Ω = 7.27×10-5 rad/s is the rotation rate of the Earth, B is the baseline length (maximum about 1.5 km), and h is the hour angle. The maximum rate is then about 0.364 ns/s, so for sample time τs = 0.833 ns we would have to step the delay once every 2.29 s for the worst case. To keep the phase of the highest channel within 1 degree, the phase correction must be updated every 2.29 s/90 = 25 ms. It appears that this worst case can be adequately handled by correcting the phase at the output of the correlator, after the 20 ms accumulation. Note also that inserting the delays in the IF causes fringe rotation (natural fringes) at a maximum fringe rate νf = (0.364 ns/s)(18 GHz) = 6.6 Hz. Averaging over a time τav = 20 ms results in an amplitude given by sinc(νfτav) = 0.97 in the worst case (18 GHz, at noon, on the longest baseline). This suggests that we might get away with applying fringe stopping at the output of the correlator as well, with a possible small amplitude correction applied. UPDATE: The correlator coarse delays will be set only on a 1 s tick, therefore the delay can be an extra ½ s early or late, giving an error in the worst case of ±0.598 ns (this is ±0.416 ns ± (½ s) (0.364 ns/s), or ±0.72τs).
Observational Procedure
The procedure for taking delay center calibration data is to track any strong interferometric point source and sweep the coarse delays in a TBD manner (i.e. track the geometric delay and apply a delay offset, and sweep the offset over some window Δτ, from – Δτ/2 to +Δτ/2) so that the phase slope across an IF band (after the corrections described above for nominal phase slope and fringe rotation) can be obtained. The delay that results in the flattest slope is the correct one. An alternative is to vector average the data over the IF band and maximize the amplitude, which would be a more sensitive measure, but could be adversely affected by RFI. This works for any band, so it should be possible to find an RFI-free band where the chosen point source is strongest. Note that the delays are antenna-based, so they have to be swept differentially (it is the difference in delay between antennas that matters). When using a cosmic source, it is enough to set one of the 27-m antennas as the reference antenna and sweep the delays of each of the others simultaneously, but an alternative is to sweep the two 27-m delays in opposite directions so that all large-small baselines can be examined separately. It is probably worthwhile to check the delays on an isolated solar active region, when available, so that small-small baseline delays can be examined. No doubt there is a clever algorithm to make sweeping of delays most efficient, so that multiple delay centers can be determined simultaneously. The duration of the calibration observation will be set by the integration time needed for an acceptable RMS deviation for the individual measurements at each delay step, and the number of steps over which the delay is swept. The delay center should be very stable, and once determined only changes to hardware or physical cables should occasion the need for remeasuring the delays. UPDATE: We have learned that on restarting a ROACH board it comes up with an indeterminate 4τs ambiguity in delay due to the sampling (ADC) clock being 4 times the FPGA clock. This means that WHENEVER A ROACH IS REBOOTED a new delay calibration is needed. A suggested methodology is to go to the Sirius XM Blues geosynchronous satellite at 115 W longitude and observe its S band (2332.5-2345.0 MHz) transmission, to determine the optimum delay by minimizing the phase slope. It will not be necessary to sweep the delay for this, however. The phase slope over 12.5 MHz will be 3.75Δn degrees, where Δn (ranging from -3 to 3 in units of τs) is the number of steps by which the delay center has changed since the previous measurement. A special pipeline procedure would be created to do the analysis and update the delay center tables. [BC 9/25/2016: We can also use strong cosmic calibrators to obtain the delay solutions.]
Analysis Procedure
In the case of delay calibration on a cosmic source with the 27-m antennas, a full delay calibration will result in 2(N - 2) + 1 measurements (27 for N = 15) to determine N - 1 (14 for N = 15) delays (one reference antenna is set to zero delay). The set of over-determined measurements can be used to find a least-squares solution. If only one delay needs to be determined (due, for example, to a hardware change affecting only one antenna), then a subarray with the one 2-m antenna and two 27-m antennas can be used, and only the affected antenna needs to be swept, resulting in 2 measurements to determine one delay. Nevertheless, it is probably good practice to measure all of the delays on some periodic schedule. In the case of delay calibration on a solar active region, with no 27-m antennas, both the delay control and analysis are more complicated. [BC 9/25/2016: Now that we only have one 27-m antenna, so our measurements are no longer over-determined: 13 measurements to determine 13 delays (it would be convenient to just set the 27-m antenna to zero delay). In practice, we can still yield plausible solutions based on observation of a strong cosmic source (e.g., 3C84).]
Table 3: Summary of Delay Calibration | ||||||
Calibration Type | Impacts Solar Observing? | Products | Uses | Control Requirements | Analysis Requirements | Priority |
Full array delay calibration on cosmic source | No | Delay pattern for each large- small baseline over an IF band | Determine optimum delay centers | Control 27-m delays in correlator (separately from geometric delay tracking) | Special analysis routine to find/solve for optimum delay solution | Essential |
Single antenna delay calibration on cosmic source | No | Delay pattern for baselines A- n and B-n,* where n is the small antenna | Determine optimum delay center for one antenna | Control 27-m delays in correlator (separately from geometric delay tracking) | Simple analysis routine to find optimum delay | Needed, could be deferred |
Full solar array delay calibration on solar active region | Yes | Delay pattern for each small- small baseline over an IF band | Verify delay centers on small-small baselines | Control all delays in correlator (separately from geometric delay tracking) | Special analysis routine to find/solve for optimum delay solution | Good to have, can be deferred |
Bandpass Calibration
Bandpass calibration refers to determining the relative complex gain and offset (system noise) as a function of subchannel across an IF band. It is measured on each large-small baseline interferometrically by observing a bright point source and integrating to obtain suitable signal-to-noise for a reliable measurement. We note that measuring the bandpass using small-small baselines is out of the question due to the low sensitivity on those baselines. The data are then analyzed to determine the resulting antenna-based complex gains. Offsets are determined by inserting full attenuation off-source, and could be considered a separate calibration, although it should be performed at the time of the bandpass calibration. Note that bandpass calibration must be measured separately for each IF band. Things that affect the bandpass are gain slopes due to frequency-dependent components/cables, higher-order ripples due to standing waves, and IF bandpass filter shape. If standard science bandwidths are used, the bandpass calibration could be done by integrating over the science subbands, to improve signal-to-noise and shorten the required duration of the observation. To maximize signal-to-noise, only large-small baselines (those with one 27-m antenna and one 2-m antenna) will be used.
Observational Procedure
The entire array tracks a bright cosmic source, one IF band at a time, integrating on each band until good signal-to-noise is achieved. The procedure is repeated for each of the 34 bands.
The sensitivity per polarization of a single baseline is given by
where and are the system temperature (K) and diameter (m) of the ith element, and an antenna efficiency of 0.5 has been assumed. If the system temperature of the cooled 27-m receivers is 30 K, and that of the 2-m receivers is 400 K, the sensitivity on baselines between a 27m-2m pair is:
it will take about 23 s with 10:1 signal to noise ratio on 3C84 on each 1-MHz-wide channel (assuming ~20 Jy flux density). Probably the higher frequency bands will have lower signal to noise, so will take longer, but these are also the bands with the wider science bandwidths. A 50:1 signal to noise ratio measurement (rms phase error about 1.1 degree) on all 34 bands can be done in 6 hours.
Analysis Procedure
The Data are calibrated to correct for pointing offsets vs. frequency (obtained from Pointing Calibration, see 1 above), and the set of amplitudes and phases on each large-small baseline are obtained. Denoting the large antennas as a, b, and the nth small antenna as n, the antenna-based bandpass amplitude as a function of subchannel k for antenna n is
where is the square of the amplitude measured on baseline i, j. There appears to be no way to measure the bandpass of the large dishes separately (without small-small baselines), but perhaps they are never needed.
Assuming we take one of the large antennas (denoted antenna a) as the reference antenna, which we can do without loss of generality, the antenna-based bandpass phase is just that measured on the a-n baseline, . Note that is useful primarily to verify phase closure. The deviation from closure phase would be used as a measure of the uncertainty in . Given sufficient signal to noise, the bandpass amplitude and phase can be determined for each subchannel k, but if that is not possible, it is sufficient to determine this calibration for each science subband. The product of this analysis is the normalized shape and relative phase variation across the band, which should change slowly (assuming thermal variations of standing waves is well controlled). The overall complex gain will be determined by more frequent measurements integrated over each entire IF band (both reference and daily gain calibration). Note that the Miriad task mfcal performs the required analysis, but no doubt assumes data for all baselines, whereas we have only a small subset of baselines. It is worthwhile to try mfcal on simulated data with some very noisy baselines to see if it comes up with a correct solution. Note also that the total power bandpass response for each antenna, obtained from section 1, could be relevant to compare with the amplitude bandpass response. [BC 2016-Sep-26: CASA's bandpass task may work on a subset of baselines. Need to be tested for only using baselines of one antenna, though.]
[BC 2016-Sep-26: Now that we only have one 27-m antenna. It means that we need to solve for the complex gain for each channel on each 2-m antenna, totaling 13 x nch solutions (where nch is # of spectral channels), from 13 x nch measurements of complex visibilities on all 13 small-large baselines. The measured visibilities can be described as:
where and are amplitude and phase of each antenna at a given spectral channel k, and and are the corresponding baseline error, or closure error. There is no over-determined measurements, unfortunately, so we have to assume no closure error and solve for the antenna-based amplitudes and phases. We also need to use the 27-m antenna as the reference and set its amplitude to unity and phase to zero for all channels.]
Table 4: Summary of Bandpass Calibration | ||||||
Calibration Type | Impacts Solar Observing? | Products | Uses | Control Requirements | Analysis Requirements | Priority |
Full spectrum bandpass calibration | No | Amplitude and phase on each large-small baseline over each spectral channel | Determine the antenna-based complex gain variations across each IF band | Relatively longer integration time on each IF band to obtain adequate SNR | Miriad task mfcal may work, CASA task bandpass may work | Needed for detailed science investigations, could be deferred |
Reference Gain Calibration
Reference complex gain calibration refers to determining the "system" amplitude and phase with high precision as a function of IF band (i.e. integrated over each 500 MHz IF band). The idea is that an observation of a calibrator for phase calibration, when corrected by the reference phase calibration, will yield a linear phase slope as a function of frequency, so that only the phase slope measurement is required for the calibration solution.
Observational Procedure
Given the speed with which a bandpass calibration (section 5) can be obtained, and the basic similarity between that and the reference calibration, the same basic observational approach can be taken, and only the analysis differs in some details. For integration over 500 MHz, the entire reference calibration can be done on 3C84 in 34 bands, at 50:1 signal to noise ratio, in less than 60 s on large-small baselines (c.f., sensitivity equations in section 5). However, it is wise to measure the reference complex gain on all baselines and seek a traditional gain solution. [BC 9/24/2016: However, optimum delay and bandpass corrections should be applied prior to averaging over these channels.]
For small-small (2m-2m) baselines, it becomes:
In principle, this permits a 10:1 signal to noise measurement on 3C84, integrated over the 500 MHz IF band, in about 100 s. [BC 9/24/2016: Again, we need perfect delay/bandpass solutions to flatten the phases before combining the channels. In reality, we would need considerably longer time to achieve this]. A one-hour reference calibration would yield a 50:1 signal to noise measurement on small-small baselines [BC: This is an ideal scenario]. Note that the 3C84 flux density spectrum has to be calibrated by reference to a calibrator standard, either 3C286 or 3C48. Both are weaker than 3C84, but only the large-small baselines are needed, so determining the 3C84 spectrum can be done in a very short time, of order 10 minutes.
Analysis Procedure
It would be fruitful to analyze separately the large-small baselines (as in section 3.2, above) to get a reference gain calibration, and the small-small baselines to get an independent calibration by traditional means, and compare. If the two are identical, then the time-consuming measurement of the small-small baselines can be abandoned except as a check on system performance. Reasons they may be different would be related to the correlation efficiency and correlator malfunction, or possibly software errors in the DPP.
Table 5: Summary of Reference Gain Calibration | ||||||
Calibration Type | Affect Solar Observing? | Products | Uses | Control Requirements | Analysis Requirements | Priority |
Band-by-band reference gain solution | No | Amplitude and phase on each small-small baseline, integrated over each 500 MHz IF band | (i) Determinetheantenna- based complex gain integrated over each IF band (ii) Compare large-small gain solution with small-small gain solution |
27-m antenna required | Standard Miriad/CASA task for antenna-based gain solution | Essential |
Daily Gain Calibration
This refers to the periodic measurements of gain calibrators during the day, and needs to be done only on the large-small baselines. A calibrator is chosen relatively nearby to the Sun, so that the local sky conditions are sampled. After correcting for the reference calibration, the phases should form a linear phase slope with frequency [BC 9/24/2016: This implies a residual multi-band delay. What is the source of this residual delay? Are we confident enough on this linearity?]. The task of the daily calibration is to obtain this phase slope as a function of time in order to permit two-point interpolation of the phase correction for intervening solar data. Note that it should not be necessary to obtain the phase in every band, unless the phase slope proves to be nonlinear. [BC 9/24/2016: But it is probably a good idea to do this for every band in the first place.]. Therefore, the phase slope can be determined over a relatively restricted range of frequencies, to avoid the problem of the widely different primary beam vs. frequency. With OVSA we observe between about 2.8 – 10 GHz. [BC 9/24/2016: How does a varying primary beam vs. frequency affect phases from a point-source calibrator?
Observational Procedure
A cosmic point source nearby to the Sun will be chosen by some automated means, and once per hour or so the array will automatically slew to the source, take data for a set amount of time sufficient for good signal to noise on selected bands, and then go back to the Sun. The distance to slew will vary depending on what frequency range is chosen for calibration, and the nearness of a suitable calibrator. Point source calibrators brighter than 4 Jy are shown in Fig. 1, from Stephen White's FASR memo on source counts.
It appears that there are plenty of sources available, with worst case slew distances of about 45 degrees. With a slew speed of 30 degrees per minute, the time off Sun is maximum 3 minutes + time on source. With a 500 MHz bandwidth, it is possible to obtain 20:1 signal to noise in each of 10 IF bands in <50 s. We also note that, although the spec of the 27-m dishes is only 18 degrees/minute, it should be possible to have them tracking the calibrator continuously. Thus, we can make a 20:1 measurement in about 5 minutes, which should permit calibrations every hour if needed.
Analysis Procedure
This calibration observation will require a specially written routine, or perhaps a script, that will average the data over the relevant 500 MHz IF bands (say 10 different bands between 2.5 and 10 GHz) on the large-small baselines, apply the reference calibration, and fit phase slopes to all of the "phase spectra." [BC 9/24/2016: Before doing this, we should test it and see if this is really the case.]. For large antennas designated a, b and small antenna n, the phases should close, i.e. , and certainly the phase slope should be forced to close. Assuming 27-m antenna a is the reference antenna, the phase slope to apply to antenna n is that fitted to the a-n baseline. The calibration should be analyzed by the pipeline immediately after the calibration is finished, so that its results can be applied immediately during the following solar scan.
[BC 9/24/2016: Shall we solve for the amplitude (per antenna, per IF) as well? Although we have corrected most of the system amplitude during reference gain calibration, there is likely time-dependent amplitude fluctuation as well.]
Table 6: Summary of Daily Gain Calibration | ||||||
Calibration Type | Affect Solar Observing? | Products | Uses | Control Requirements | Analysis Requirements | Priority |
Daily phase calibration in 10 (or so) IF bands | Yes | Phase in each IF band on each large- small baseline, integrated over each 500 MHz IF band | Determine the linear phase difference since the last reference calibration | 27-m antenna required; Possibly requires subarray coordination if 27- m are to track cal source continuously | Special routine or script | Essential |


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- Digital copy (scan) of the passport's biographical page.
- You can use a credit or debit card to cover the processing fee.
The Indian government has taken steps to boost the tourism industry in India. One such measure is the implementation of the Indian e-Visa, which aims to attract tourists from around the world. Since 2014, South Africans can apply for Indian visas online. They can obtain an e-Visa to visit India. Citizens of 169 countries may apply for an e-Visa to India based on the purpose of their visit. If you plan to visit India, you must first obtain an e-Visa for Indian tourists. Holders of an e-Tourist Visa can stay in India for up to 30 days from the date of entry, with a limit of one entry and no extensions. On the other hand, if you are visiting India for business purposes, you will need an India Business eVisa. Using an e-Business Visa, you can stay in India for 365 days with multiple entries. However, this type of visa does not allow you to stay longer than 180 days at a time. If the traveler is visiting the country for medical treatment, they must apply for an Electronic Medical Visa. e-Medical Visa: Stay in India for 60 days from the date of entry into India with triple entry. Applying for an India e-Visa is a very simple process that is completed online and saves travelers the hassle of going to a local embassy or consulate to apply for one.
- Tourist eVisa.
- Business eVisa.
- Medical eVisa.
Required Documents for South Africans Citizens
- All travelers must have a passport that will be valid for at least 6 months from the date of their arrival in India.
- A valid payment method (such as your debit/credit card) to pay for the eVisa fees.
- A digital photo of yourself (it must have been taken recently, you cannot make any gestures, and it must have a white background).
- A valid email address to receive the eVisa in their Inbox.
Traveling to India is an unforgettable experience because there are so many diverse landscapes and cuisines to sample. India has it all: vast national parks, wildlife safaris, white sand beaches, fascinating religious sites, as well as numerous traditional festivals, massive temples, caves, forts, and sculptures. Since 2014, the Indian government has made the Indian visa available online for Israeli citizens. Citizens of 169 countries can now apply online for an Indian visa. The number of visitors to India has risen dramatically in recent years, especially since the introduction of the India e-Visa in 2015. Israeli passport holders must obtain an e-Visa before traveling to India. Israeli citizens can travel to India with an India Tourist eVisa to see friends and family and take part in activities like yoga retreats. The India Business eVisa permits sales, business meetings, employment placement, and other business-related activities. Finally, the Indian e-Medical Visa allows you to get medical care in India. The three types of Indian visas for Israeli citizens have different validity periods and the number of entries allowed is: Tourist e-Visa: Double entry for up to 90 days with a validity of one year. Electronic Business Visa: double entry for a maximum of 180 days with a validity of one year. Electronic Medical Visa: triple entry for a maximum of 60 days. With the eVisa for India, the application process for citizens of Israel and other eligible countries has been greatly simplified as all documents can be submitted online.
Types of eVisa for citizens of Israel
- Tourist eVisa
- Business eVisa
- Medical eVisa
Required Documents for Israeli Citizens
- Their Israel passport, valid for at least six months from the date of entry in India.
- A valid email address where the Indian eVisa will be sent.
- A credit or debit card to pay for the eVisa fee.
- A digital copy of the biographical page of the passport.
- A recent passport-style color photo of the Israeli passenger.
Disclaimer: The views, suggestions, and opinions expressed here are the sole responsibility of the experts. No journalist was involved in the writing and production of this article.


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As millions of dollars flood into relief efforts for the Boston bombing victims, donations to devastated West, Texas, are lagging far behind.
More than $26 million has been raised in the wake of the April 15 Boston blasts. And it appears that donations for West total well under $1 million.
The Salvation Army, for example, has raised about $200,000 following the April 17 fertilizer plant explosion that killed 14 people, injured up to 200 and destroyed more than 100 homes. It has already spent about the same amount.
The needs in 2,800-person West are vast: food, shelter and transportation for displaced families, medical help for blast survivors, and eventually assistance rebuilding an entire community -- from houses and businesses to a school and nursing home. Property losses alone are expected to exceed $100 million, according to the Insurance Council of Texas.
CNN's Impact Your World: How you can help
Dan Ford, a resident of nearby Waco and the head of the McLennan County Salvation Army, understands the outpouring of support for Boston. But he said West is suffering.
"We've been greatly overshadowed by the Boston tragedy," said Ford. "We need help."
Another local group, the West, Texas Disaster Relief Efforts Fund has raised about $140,000.
Ashley Allison, executive director of the Waco Foundation, which helped establish the fund, said some of the largest donors indicated they gave because the media isn't paying enough attention to West.
"Families are hurting no matter how much media coverage is given," said Allison.
Meanwhile, Baylor University's West Relief Fund has collected a little more than $110,000, and another $50,000 has been raised between the United Way of Tarrant County, the Society of St. Vincent dePaul's and the National Fallen Firefighters Foundation.
The American Red Cross, as it does in most cases, is accepting general donations, some of which will be directed to West. It hasn't yet released an estimate of how much it has spent.
Related: Before and after: West, Texas plant explosion
GiveForward, a crowdfunding platform where anyone can set up a campaign and solicit donations for a cause, has been used for both of last week's tragedies.
But the site has had more than 24 crowdfunding initiatives pop up for Boston, raising $1 million so far -- compared to only six initiatives for West that have raised a mere $5,000.
The majority of the $5,000 raised on GiveForward for West victims has been dedicated to medical bills for a 2-year-old Texas survivor, Arianna Gassaway.
"Arianna has very extensive injuries including multiple broken bones, numerous lacerations and a severe head injury," the fundraiser says.
The $4,314 raised for Arianna so far is only 9% of her family's $50,000 goal.
Ethan Austin, co-founder and president of GiveForward, said the discrepancy between fundraising efforts for Boston and West likely has a lot to do with the differing emotions behind the giving.
"The explosion in Texas was an accident. The reaction was sadness. The bombings in Boston were a heinous and malicious act that brought back memories of 9/11. The reaction was anger," he said. "Stories inspiring high energy emotions like anger have a much higher likelihood of going viral. Stories inspiring low-energy emotions like sadness do not tend to go viral."
And as the media continues to focus intensely on the Boston bombing victims and suspects, people aren't hearing nearly as much about the devastation in West, said Stacy Palmer, editor of the Chronicle of Philanthropy.
"When you see a disaster get a lot of attention, you see a lot of giving ... and you really don't see as many stories that show the picture of what's happening [in Texas]," said Palmer.


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CeeLo Green Cuts Performance Short, Promoter Refuses to Pay
CeeLo Green said "forget you" to an audience in Little Rock, Ark., on Saturday (May 24) when he cut a performance incredibly short, angering the promoter and disappointing fans.
According to TMZ, Cheddy Wigginton, who sits on the board of Riverfest -- the festival at the center of this whole mess -- said the singer was contractually obligated to perform for 75 minutes, but he left the stage just after 40, reneging on the previously agreed upon set time. And on top of that, CeeLo showed up 35 minutes late.
The agreement also stipulated that the Goodie Mob member would get half of the money up front, which was about $50,000, and the rest would be given to him after completing his set. Although he was given a check for the remaining $50,000, Wigginton eventually canceled it.
So far, CeeLo hasn't responded to the promoter's claims. Also, Wigginton didn't say he would pursue the matter further, however, that doesn't mean he won't.
The day following the show, CeeLo sent out a tweet about Riverfest, revealing he had an "amazing" time.


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