Heat 2 tsp of ghee in a kadai. Once the ghee is hot enough, simmer the flame and roast cashew nuts and raisins. Once the raisins balloon up, remove. Then roast the grated coconut. Remove once done. Keep all these aside.
In a bowl, take all the roasted Rava, Nuts, Coconut and add the Cardamom powder. Then add the sugar. Mix well.
Then slowly add the warm milk into the bowl. Check if you are able to gather as balls. When you find that milk added is enough to get you laddos, transfer it back to the kadai and cook in sim for 2 mins. Mix well and then cover it and let it rest for 2 mins. Then immediately make balls or laddoos.
Enjoy the delicious rava laddoooss!!!!
Heat a tsp of oil and saute the chopped onions until they turns transparent...Smash the cooked chickpeas and dip the bread slices in water,squeeze out the excess of water and smash it.. Take both the smashed chickpeas, bread slices with sauteed onions, garam masala powder, chilly powder, chopped bell peppers, fennel seed powder , coriander leaves and salt..mix everything well and make out medium size rolls, meanwhile preheat the oven at 250F..
Arrange a baking sheet over a baking tray, brush the baking sheet with oil, place the rolls over the greased baking sheet one by one by leaving spaces between each rolls..Brush the rolls with few drops of oil and bake for 30 minutes by turning the roll on both sides until they turn slightly brown..
Serve hot with any hot n spicy sauce!!
Mix together the flour, salt, anise seeds, sesame seeds,sugar, yeast with ur fingers, slowly add the warm water and olive oil, slowly turn the flour as dough, knead slowly for 15minutes until they turns very soft and smooth...Divide the dough as two equal dough...flatten the dough and keep in a warm place covered with a towel for 45 minutes..if you touch the surface the uncooked dough will comes back, now the dough is ready to bake...springle some flour over the baking tray and arrange the raised dough over the flour, poke the dough with fork..
Preheat the oven at 400F, arrange the baking tray in the middle of the oven and bake the bread for 30-40minutes..
Enjoy the freshly baked bread!
Serve hot with hot rice!
Spinach is a leaf vegetable which grown in the temperate regions of the world. It is green in color and is a good source of iron and calcium. There are three main types of the vegetable: Savoy, smooth leaf and semi-savoy. Savoy has dark green, crinkly and curly leaves and is the most common type available in supermarkets. Smooth leaf has smooth, broad leaves that make it easier to clean than the savoy variety. This type is usually grown for use in canned and frozen spinech and soups. Semi-savoy is a hybrid with slightly crinkled leaves and the same texture as savoy, but it is not so tricky to clean.I do often prepare dishes with spinach greens from dals to stir fries but never tried to make breakfast dishes with spinach green, after a long hesitation i added few spinach leaves grinded with green chillies, ginger pieces and coriander leaves to the left over idly batter to make out as spinach dosas, i prepared as mini dosas and the little ones at home like it much with vegetable kurma..even for my surprise, everyone at home liked much this green dosas..
Grind together the chopped spinach leaves, ginger pieces, green chillies and chopped coriander leaves into fine paste, add this paste to the idly batter and add a quarter cup of water and mix everything well..heat a non stick pan, grease the pan with oil and paper towel or with a slice of onion..now pour a spoonful of batter and turn in clockwise to small circles..drizzle few drops of oil around and flip the other side and cook well..Serve hot..
Grind everything from the list 'To Grind' as fine paste and keep aside...heat enough oil and add the whole spices, fry them until they turns brown, add the chopped onion pieces, tomato pieces, garlic paste, ginger paste and cook everything until the oil get separates, add immediately the mixed vegetable and saute everything until the veggies turns bit tender...add the already grounded paste to the veggies and stir everything well, add enough salt to the gravy also add enough water to the gravy as per ur need..cook everything in medium flame until the veggies get well cooked..finally add the mint leaves and put off the stove..
Serve hot as side dish with hot spinach dosas!!!!..
Bring water to boil and add the green chillies, let them cook until the flavours comes out, put off the stove and pass immediately the cooked green chillies to cold water, bring boil together the rice vinegar, salt and sugar and add the cooked green chillies to the vinegar and put off the stove...Leave it for atleast 3hours aside before serving, if its too vinegary, stir a spoon of sugar to the pickled green chillies..
Grease a bowl and pour the idli batter to half of the bowl, add a tablespoon of masala, pour again the idli batter to cover the masala, cook in microwave for 5 minutes in high..insert a toothpick to check whether the idli is well cooked, if its come out clean, the idli is prefectly cooked..
Heat enough oil and add the mustard seeds, urad dal, cumin seeds, dry red chillies and asafoetida powder and let them splutters, add the chopped onions, chopped tomatoes, slit opened green chillies and crushed garlic cloves, saute everything until the onions turns transculent...add the cooked dal with enough water and salt..cook until the oil gets separates, finally add the lemon juice and chopped coriander leaves and put off the stove..
Enjoy the delicious tomato sambhar with microwave stuffed vegetable idli!!!!
Bhel puri is a puffed rice dish with potatoes and a tangy tamarind chutney..its a type of chaat particularly identified with Mumbai beach...Bhelpuri is prepared across India with many different names...The ingredients include diced boiled potatoes, tamarind and dates chutney,with sev, chopped onions, chopped tomatoes etc..Bhelpuri was originally from Gujarat and its a fast food item, later they got merged with mumbai culture and became synonymous with Mumbai..There are two popular chutneys are used to prepare this bhelpuri, one is dark sweet chutney made mainly with dates and tamarind and the another one is spicy green chutney made with coriander leaves and green chillies...I went once to Mumbai, but i have tasted few mumbai chaat foods since am a great fan of chaat foods.
Mix everything in a large bowl and serve immediately in a small snacks plates... else the juice from tomatoes, cucumber may turns this bhel puri soggy..Enjoy!!!
Heat enough oil and add the cumin seeds, coriander seeds, fennel seeds, let them splutters..add immediately the chopped onion and fry until they turns transculent..Add the boiled potatoes with red chilly powder, turmeric powder and salt...Fry in simmer until the oil get separates...finally add the dry fenugreek leaves and toss gently...cook for few seconds and put off the stove..
Enjoy the alu fry with any sort of rice dishes!!!
Mix the yeast with quarter cup of luke warm water , sugar and salt...let it sit for 5 minutes until they turns foamy.. Mix together the semolina flour and all purpose flour, make a well and add the foaming yeast ,oil, water to form a dough..the dough should be soft but not sticky...knead the dough for few minutes and divide the dough as 5-6 medium sized balls , roll each ball into thin circles, arrange the rolled dough in a clean and dry towel and leave to rise for 1 hour..after an hour the rolled dough would have doubled their volume..
Heat a lightly oiled iron skillet or non stick pan, cook the batbout on turning several times, cook in simmer for few minutes until they turns golden brown on both sides and arrange in wire rack to get cool a bit...batbout can be served bit warm too..
Enjoy the batbouts with any sort of dips and spreads!!!
Heat enough oil and add the cumin seeds, let them splutters..add the onion slices and saute until its turns transculent, now add the mixed vegetables and stir with red chilly powder, cumin seed powder, pepper powder, garam masala powder, coriander leaves with enough salt...meanwhile grind the chopped tomatoes as puree..heat few drops of oil in a small pan and shallow fry the paneer cubes until they turns golden brown, keep aside...once the veggies are half cooked, add the freshly grounded tomato puree and cook everything in medium high flame until the oil get separates...Finally add the cooked rice and fried paneer cubes to the cooking veggies , toss gently until everything get well mixed..
Garnish the ginger chilli shrimps with chopped green onions and serve with hot rice!!!
Crêpes the famous french pancakes are made by pouring a thin liquid batter into a hot frying pan or flat circular hot plate, often with a trace of butter or oil on the pan's surface. The batter is spread evenly over the cooking surface of the pan or plate either by tilting the pan or by distributing the batter with an offset spatula.
Common savoury fillings for meal crêpes include: cheese, asparagus, ham, spinach, eggs, ratatouille, mushrooms, artichoke in certain regions, and various meat products.When sweet, they can be eaten as dessert. They can be filled with various sweet toppings, often including Nutella spread, sugar granulated or powdered, maple syrup, lemon juice, whipped cream, fruit spreads and sliced soft fruits.Here is my version of serving my french pancakes with strawberry chunks marinated with few teaspoons of Strawberry jam and few tablespoons of whipping cream, I dont think nothing will beat when compared to this delicious dessert also fulfilling snacks for school returning kids..
Mix the flour, chilly powder, soya sauce, vinegar, ginger pieces,green chilli pieces garlic pieces and salt..add the chicken pieces to this marination and marinate it for atleast 4hours in fridge..heat the oil in a fry pan and add the onion, saute till they turns slightly golden, now add the marinated chicken pieces, capsicum pieces and saute in low heat for few minutes until the chicken get cooked...garnish with coriander leaves and serve..
Blend together the fresh mango chunks, dates syrup and ice cubes...Serve immediately and enjoy the healthy and fresh juice!!
Sesame seeds contain sesamin and sesamolin, substances that is believed to prevent high blood pressure and protect the liver against damage.Sesame seed is a good source of Vitamin E, that is why it can help strengthen the heart and the nervous system.Half cup of sesame seeds contains 3 times more calcium than half cup of whole milk.Unhulled sesame seeds can be stored in an airtight container in a cool, dry, dark place. Once the seeds are hulled, they are more prone to rancidity, so they should then be stored in the refrigerator or freezer.Add sesame seeds into the batter the next time you make homemade bread, muffins or cookies.Combine toasted sesame seeds with rice vinegar, tamari and crushed garlic and use as a dressing for salads, vegetables and noodles.We know very well that spinach have loads of health benefits, I prepared spicy and delicious savoury buns with frozen spinach, crushed garlic, red chilly flakes, quick cooking oats, sesame seeds, flax seeds, store bought fried onions...Its such a healthy and delicious spinach buns suits prefectly even when u go for picnics, this savoury buns can be served with herbed creamy cheese for a quick dinner with any sort of soups...We enjoyed having this sesame and spinach buns with cheese and salad filling..
Combine in a cup of luke warm water, the active dry yeast, salt and sugar..let it sit for 5 minutes..Take the all purpose flour, whole wheat pastry flour, quick cooking oats, flax seeds, sesame seeds, frozen and thawed spinach, redchilly flakes, fried onions, crushed garlic cloves, olive oil and mix everything well..gradually add the foamy yeast with half a cup of luke warm water, knead as dough...dust the dough with enough flour and knead for few minutes until its turns soft..arrange the dough in a greased bowl , let it sit for an hour in a warm place..
Once the dough doubled their volume, make 6balls from the dough and roll them as buns...Arrange the buns in a baking sheet and let it sit again for an hour...Brush the buns with olive oil and springle the sesame seeds over the buns...Preheat the oven for 350F..
Arrange the unbaked buns in middle rack of the oven and bake for 30 minutes or until the buns turns golden brown...Enjoy the savoury buns!
Heat few drops of olive oil, add the chopped tomato pieces, chopped spinach and saute until the spinach shrinks,tomatoes turns mushy..keep aside..add the quarter cup of vegetable stock to the cooked tomatoes and spinach , grind everything as coarse puree..
Before serving, garnish a teaspoon of cream and enjoy the hot soup!!!
Focaccia is a style of bread made popular in Italy, and spreading around the world wherever Italian settlers and traders have formed communities. The bread is relatively flat, usually quite plain inside, but topped with olive oil and herbs, and occasionally with sliced olives on top. A range of varieties of focaccia exist, and in the 21st century new varieties have been created due to the versatility of the basic recipe.focaccia is slightly different in that the loaf does rise slightly so is not a traditional unleavened bread, and the focaccia recipe is mostly unknown in the Middle East, yet has a history of being prepared in Turkey, Greece, Italy, France, and Spain.Focaccia is no longer strictly the preseve of Italian communities, nowadays it can be found in almost all bakeries and supermarkets. With a wide variety of seasonings, focaccia bread makes a very tasty sandwich bread, and is frequently served with cheese fillings.I have already prepared Olive Basil Focaccia and Onion Focaccia and here comes my another focaccia bread with chopped mushrooms and grated emmental cheese..
Mix the sugar, salt n yeast in luke warm water n let them sit for 5 minutes.. meanwhile take the all purpose flour in a mixing bowl n add the foaming yeast, mix everything well, its will be stickly at this point, transfer them to lightly floured surface n knead for a while until they turn soft dough..
Coat a deep bowl with olive oil n place the soft dough also brush with more oil, cover it n let it rise for 1 hour in a warm place..After an hour it will almost doubled the size...Grease few drops of oil to the baking pan n press the dough to flatten them, springle the chopped mushrooms over the dough and let them sit again for 1 hour..
The dough will again rise n double in sizen now springle the grated cheese over the dough....Preheat the oven to 475F, place the baking pan in middle rack n bake for 20 minutes r else until the dough turns slightly brown..
Heat few drops of sesame oil, add the paneer cubes and fry on both sides until they turns golden brown..add the chopped onions, garlic cloves, saute for few minutes..add immediately the bell pepper pieces, soya sauce, rice vinegar, salt, chilly sauce, tomato sauce and give a stir...cook in medium high flame until the bell peppers turns slightly tender...add now the shallow fried paneer cubes and give a stir...cook everything for 2 minutes and put off the stove..
Garnish the chilly paneer with chopped green onions..Serve hot!!!
Preheat the over to 425F..in a bowl combine the flour, baking powder, sugar and mix, add the small cubes of butter and mix until they turns as coarse meal...transfer the mixture to a large bowl and make a well, pour the milk..with a fork stir everything gently, dont stir for a long...grease a cake pan and flour it, pour the batter and bake of 10 minutes or until risen and golden brown...remove from the pan and slice the biscuit as u desire...arrange few strawberries and whipping cream as ur desire and serve it!!
Take a cup of luke warm water and add the yeast, salt and sugar..mix well and let it stands for 5 minutes until the yeast turns foamy...Mix the semolina flour, white flour and take the flours in a large vessel, make a well in the centre of the flours and add the foamy yeast..Add the oil and warm water to the flour and mix everything well with ur fingers..
Now preheat the oven to 435F (225°c)..poke the dough with a fork and bake the bread for 20 minutes in middle rack until the bread are nicely coloured and sound hollow when tapped...Transfer the bread to a rack and let it cool..
The recipe for 'Fondue' came from Switzerland. The name is French but the dish originated in 'Switzerland'. The Swiss are fond of all fondues but especially of cheese fondue, which is had with crusty bread especially in the winters to keep off the cold. Many explanations was given for why a French name was given for a Swiss dish have been discussed. Various people have come up with different explanations. The chefs have their own glossary which says Fondue means simply 'to melt' in French..Seems the Swiss are very poor at naming their dishes and only good at making the finest and best cheese in the world. Initially i want to try swiss cheese fondue, but once i saw the chocolate fondue i really got hooked with this fondue and tried out at home..We had with marshmallows, u can serve very well with any sort of fruits.We just enjoyed this chocolate fondue sterday...Am sending this swiss chocolate fondue to AWED-Swiss guest hosted by Sweatha, event by DK..
Melt the chocolate pieces along with the cream and vanilla essence in thick bottomed pan over low hear stirring continuously till it comes to a boil and then reduce the flame and keep stirring for another 5 minutes. Then remove the pan from the flame and allow the mixture to cool a bit, then pour it into a fondue pot or ceramic dish and serve.
Serve with any sort of fruit pieces or marshmallows!!!
Grease a ramekin or small bowl with melted butter and add the water, now add the egg with pinch of salt n pepper..sprinkle the grated cheese and chopped green onions over the egg and cook in high for 2minutes in microwave oven,take off the poached egg from the ramekin and serve immediately with toasted bread slices..
While serving springle confection's sugar and chocolate powder over the jelly and serve it!!!!
Take the cooked dal water, crushed garlic cloves, crushed tomatoes, home made rasam powder, water with enough salt together in a bowl ....heat enough oil and add the mustard seeds, cumin seeds, dry red chillies and asafoetida powder and let them fry..add immediately the chopped methi leaves and saute until they shrinks..now add the dal-spice water..once they starts bubbling, keep in simmer and cook for 2 minutes, finally add the lemon juice and chopped coriander leaves and put off the stove..
Serve hot with moroccon breads!!!
Serve the mango sorbet as scoops and garnish with few almond flakes!!!
Cut the potatoes as cubes, heat the oil and add the cumin seeds and let them splutters, add the cubed potatoes and cook in simmer for few minutes..add the red chilly powder, turmeric powder and salt..springle some water and cook until the potatoes get well cooked..
Serve hot with rice and any gravies!
Peel and chop roughly the sweet potato, cook until they get well cooked in enough water and salt...drain the cooked water and mash the cooked sweet potato pieces, heat a few spoon of oil and cook the chopped onion until they turns transculent...mash coarsely the canned chickpeas..now add the cooked onions, mashed chickpeas, red chilly powder, fennel seed powder, garam masala powder and salt to the already cooked sweet potato pieces and turn them as dough..
Make 10-12 balls and flatten it as cutlets..Mix the corn flour with enough water as white paste..dip each cutlets in white sauce and roll it evenly in bread crumbs, fry as shallow frying until both sides of the cutlets turns brown...drain the excess of oil in a paper towel..
Serve hot! am sending this delicious cutlets to Lore's Original Recipes..
Muesli is a popular breakfast cereal based on uncooked rolled oats, fruit and nuts. It was developed around 1900 by Swiss physician for patients in his hospital..Packaged muesli is a mixture of mainly rolled oats together with various pieces of dried fruit, nuts, and seeds. It commonly contains other rolled cereal grains such as wheat or rye flakes...While the fresh muesli are prepared by using dry rolled oats or whole grain oats that have been soaked in water or fruits juice..can also add grated or chopped fresh fruits or else dried fruits and with milk products like yogurt, cream, cottage cheese etc...U can also prepare ur fresh museli with spice powders like cinnamon, ginger powder and also with few seeds...Here is my simple, easy and best way to indulge this muesli by turning them as bars with marshmallows, chocolate powder.. i prepared this bars in microwave and the preparation time takes just 7minutes...These bars goes directly to MEC-Breezy Breakfast guest hosted by Simran of Bombay Foodie, event started by Srivalli, also sending to Divya's Show me your Breakfast and finally to EFM June- Breakfast & Variety rice series by Srilekha..
Heat the marshmallows, chocolate powder n butter together in a microwave bowl for 7 minutes, r until the marshmallows get completely melted...whisk them well with a spatula n add immediately the muesli...grease a pan n spread this marshmallows-muesli mixture, let them cool..cut them as any shapes as ur desires n store them in air tightened box..


Quality will never be a problem with this desk because it is made of medium fiberboard construction. The inner top finish of the desk is of laminate walnut while the outer finish is laminated black color. The desk comes in a wall leaning design, thus you can easily occupy the empty wall space you have at home. Along with the package is a heavy-duty wall fixture patches you can use to the desk will be installed still and safe for you to use. The desk features lean chrome plated legs giving it an airy and light appearance.
A little assembly with two adults is required for this furniture piece and cleaning is dead easy by wiping clean the desk using a damp cotton cloth. The Enitial Lab Modern Leaning Office Desk is made in Taiwan and measures 43 inches wide by 16 inches deep by 48 inches high. [CLICK HERE to get more details about Enitial Lab Modern Leaning Office Desk].


text:
Core Investment Companies
(Updated as on December 20, 2016)
The Reserve Bank of India is entrusted with the responsibility of regulating and supervising the Non-Banking Financial Companies by virtue of powers vested in Chapter III B of the Reserve Bank of India Act, 1934. The regulatory and supervisory objective, is to:
a) ensure healthy growth of the financial companies;
b) ensure that these companies function as a part of the financial system within the policy framework, in such a manner that their existence and functioning do not lead to systemic aberrations; and that
c) the quality of surveillance and supervision exercised by the Bank over the NBFCs is sustained by keeping pace with the developments that take place in this sector of the financial system.
Over last some years, RBI has carved out some specialized NBFCs like Core Investment Companies (CICs), NBFC- Infrastructure Finance Companies (IFCs), Infrastructure Debt Fund- NBFCs, NBFC-MFIs and NBFC-Factors being the most recent one.
It has been felt necessary to explain the rationale underlying the regulatory changes and provide clarification on certain operational matters for the benefit of the NBFCs, members of public, rating agencies, Chartered Accountants etc. To meet this need, the clarifications in the form of questions and answers, is being brought out by the Reserve Bank of India (Department of Non-Banking Supervision) on Specialized NBFCs with the hope that it will provide better understanding of the regulatory framework.
The information given in the FAQ on Systemically Important Core Investment Companies (CICs-ND-SI) is of general nature for the benefit of the public and the clarifications given do not substitute the extant regulatory directions/instructions issued by the Bank to the specialized NBFCs.
Core Investment Companies (CICs)
1. What is a Systemically Important Core Investment Company (CIC-ND-SI)?
Ans. A CIC-ND-SI is a Non-Banking Financial Company
(i) with asset size of Rs 100 crore and above
(ii) carrying on the business of acquisition of shares and securities and which satisfies the following conditions as on the date of the last audited balance sheet :-
(iii) it holds not less than 90% of its net assets in the form of investment in equity shares, preference shares, bonds, debentures, debt or loans in group companies;
(iv) its investments in the equity shares (including instruments compulsorily convertible into equity shares within a period not exceeding 10 years from the date of issue) in group companies constitutes not less than 60% of its net assets as mentioned in clause (iii) above;
(v) it does not trade in its investments in shares, bonds, debentures, debt or loans in group companies except through block sale for the purpose of dilution or disinvestment;
(vi) it does not carry on any other financial activity referred to in Section 45I(c) and 45I(f) of the RBI act, 1934 except investment in bank deposits, money market instruments, government securities, loans to and investments in debt issuances of group companies or guarantees issued on behalf of group companies.
(vii) it accepts public funds
2. Will existing Core Investment Companies (CICs) which had previously been exempted from registration and whose asset size is less than Rs. 100 crore again be required to submit application for exemption?
Ans: Existing CICs which were exempted from registration in the past and have an asset size of less than Rs 100 crore are exempted from registration in terms of section 45NC of the RBI Act 1934, as stated in Notification No. DNBS.(PD) 220/CGM(US)-2011 dated January 5, 2011, and as such are not required to submit any application for exemption.
3. Would existing CICs which had previously been exempted from registration and whose asset size is less than Rs. 100 crore be required to submit Statutory Auditor's Certificate with reference to position as on March 31 of each year to the effect that the company continues to comply with the earlier norms based on which it was treated as a 'Core Investment Company'.
Ans: No, Existing CICs which have been exempted from registration in the past and have an asset size of less than Rs 100 crore are exempted from registration as stated in Notification No. DNBS.(PD) 220/CGM(US)-2011 dated January 5, 2011. As such they are not required to submit any auditor's certificate that they comply with the requirements of the Notification.
4. A single group is having under its fold four to five prospective Core Investment Companies with an aggregate asset size of more than Rs. 100 crore. In such a situation, which company among the group companies is required to seek registration as CIC with the Bank.
Ans: All companies in the group that are CICs would be regarded as CICs-ND-SI (provided they have accessed public fund) and would be required to obtain a Certificate of Registration from the Bank.
5. A single group is having under its fold various prospective Core Investment Companies with an aggregate asset size of more than Rs. 100 crore. One of the entities has raised / holds public funds (one of the pre requisites for qualifying as a CIC-ND-SI). In such a situation, whether every CIC within the group or only the parent CIC or the specific entity that has raised/ holds public funds would be regarded as CIC-ND-SI, and thus would be required to seek registration as CIC-ND-SI with the Bank.
For Example: HCo is the parent group CIC holding 100 per cent equity capital of A, B and C, all of which are also CICs . In case C has accessed public funds, whether HCo as well as A, B and C must seek registration as CIC-ND-SI or will just C need registration?
Ans: In such a case only C will be registered, provided C is not funding any of the other CICs either directly or indirectly.
6. Whether the investment of a company in its subsidiary's subsidiary (step down subsidiary) will be taken into account for determining not less than ninety percent of its net assets.
Ans: All direct investments in group companies, as appearing in the CICs balance sheet will be taken into account for this purpose. Investments made by subsidiaries in step down subsidiaries or other entities will not be taken into account for computing 90 percent of net assets.
7. Would Current Liabilities also form part of Outside Liabilities? What will be the treatment of DTL, Advance Tax Due and Provision for Income Tax? Will they be Outside Liabilities?
Ans: Anything that has to be repaid will be an outside liability.
8. In case an existing NBFC-ND-SI is converted into a CIC-ND-SI after fulfilling the stipulated criteria, will the existing CoR continue or will a fresh application need to be made?
Ans: As there would be a separate application form for CICs-ND-SI, they would have to apply afresh.
9. What items are included in the 10% of Net assets which CIC's/CIC's-ND-SI can hold outside the group?
Ans: These would include real estate or other fixed assets which are required for effective functioning of a company, but should not include other financial investments/loans in non group companies.
10. Is there an enabling provision for use of statutory accounts based on some date other than 31st March, such as December 31st?
Ans: While such accounts could be taken into account in view of the fact that developments after balance sheet date are also taken into account, all NBFCs including CICs-ND-SI would mandatorily have to finalise their accounts as on March 31 of the year, and submit annual auditors certificate based on this figure.
11. Whether investments in a group entity other than a Company, say partnership firms, LLPs, Trusts, Association of Persons, etc by CICs-ND-SI could be regarded as investments in Group Companies for the purpose of calculating 90% investment in Group Companies.
Ans: No, only investments in companies registered under Section 3 of the Companies Act 1956 would be regarded as investments in Group companies for the purpose of calculating 90% investment in Group companies. Moreover, CICs are prohibited from contributing capital to any partnership firm or to be partners in partnership firms including Limited Liability Partnerships (LLPs) or any association of person similar in nature to partnership firms.
12. Are CICs-ND-SI exempt from the Systemically Important Non-Banking Financial (Non-Deposit Accepting or Holding) Companies Prudential Norms (Reserve Bank) Directions, 2015?
Ans: No, they are only exempt from norms regarding submission of Statutory Auditor Certificate regarding continuance of business as NBFC, capital adequacy and concentration of credit / investments norms.
13. Would CICs-ND-SI require NOC in terms of Regulation 7 of FEMA (Transfer or Issue of Any Foreign Security) Amendment Regulations Act 2004 in case they want to invest abroad?
Ans: Yes, as they are regulated by RBI, they would require NOC from Department of Non-Banking Supervision (DNBS) for making investments in the financial sector. However, a registered CIC making investments in the non-financial sector need not obtain prior approval from the Department of Non-Banking Supervision (DNBS), RBI. It will only need to report such investments to the Department within 30 days of such investment.
14. Do CICs which are exempt from registration, and investing overseas need NOC from DNBS?
Ans: Exempted CICs desirous of making overseas investment in financial sector shall first need to hold a Certificate of Registration (CoR) from Reserve Bank of India (the Bank) and will have to comply with all the regulations applicable to registered CIC-ND-SI. However, they need not obtain NOC from the Bank if their investments overseas are in the non-financial sector.
15. Whether NBFCs already registered with the Bank as category "B" company whose asset size is below Rs. 100 crore, but fulfilling the CIC criteria, can seek voluntary deregistration (as such companies are not otherwise required to get registered with the Bank under the new norms)? If so, which source should be relied upon viz certificate from Statutory auditor or audited balance sheet for one year or more?
Ans: Yes, CICs presently registered with the Bank but fulfilling the criteria for exemption under Notification No 220 dated January 05, 2010 can seek voluntary deregistration. Both audited balance sheet and auditors certificate are required to be submitted for the purpose.
16. Whether CICs having asset size below Rs. 100 crore are regulated by the Reserve Bank?
Ans: CICs having asset size of below Rs 100 crore are exempted from registration and regulation from the Reserve Bank, except if they wish to make overseas investments in the financial sector.
17. As per the definition of CIC, only investment/loans/debt in group companies is eligible for computing 90% exposure? What treatment is to be given to company's investment in group's partnership concerns?
Ans: CICs are prohibited from contributing capital to any partnership firm or to be partners in partnership firms including Limited Liability Partnerships (LLPs) or any association of person similar in nature to partnership firms.
18. If a company is unlisted, would the terms of block deals apply? What is the minimum number/value of shares transferred for it to be defined as a block deal/block sale?
Ans: The term used in the CIC circulars is block sale and not block deal which has been defined by SEBI. In the context of the circular, a block sale would be a long term or strategic sale made for purposes of disinvestment or investment and not for short term trading. Unlike a block deal, there is no minimum number/value defined for the purpose.
19. Can CICs/CICs-ND-SI accept deposits?
Ans: No, CICs/ CICs-ND-SI cannot accept deposits. That is one of the eligibility criteria.
20. What does the term public funds include? Is it the same as public deposits?
Ans: Public funds are not the same as public deposits. Public funds include public deposits, inter-corporate deposits, bank finance and all funds received whether directly or indirectly from outside sources such as funds raised by issue of Commercial Papers, debentures etc. However, even though public funds include public deposits in the general course, it may be noted that CICs/CICs-ND-SI cannot accept public deposits.
21. In the definition of public funds, what do the term "indirect receipt of public funds" mean?
Ans: Indirect receipt of public funds means funds received not directly but through associates and group entities which have access to public funds.
22. Can CICs issue guarantees and will this be considered part of definition of public funds?
Ans: Yes, CICs may be required to issue guarantees or take on other contingent liabilities on behalf of their group entities. Guarantees per se do not fall under the definition of public funds. However, it is possible that CICs which do not accept public funds take recourse to public funds if and when the guarantee devolves. Hence, before doing so, CICs must ensure that they can meet the obligation there under, as and when they arise. In particular, CICs which are exempt from registration requirement must be in a position to do so without recourse to public funds in the event the liability devolves. If unregistered CICs with asset size above Rs. 100 crore access public funds without obtaining a Certificate of Registration (CoR) from RBI, they will be seen as violating Core Investment Companies (Reserve Bank) Directions, 2011 dated January 05, 2011.
23. What is a Group company?
Ans: For the purposes of determining whether a company is a CIC/CIC-ND-SI, 'companies in the group' have been exhaustively defined in para 3(1) b of Notification No. DNBS. (PD) 219/CGM(US)-2011 dated January 5, 2011 as "an arrangement involving two or more entities related to each other through any of the following relationships, viz.,Subsidiary – parent (defined in terms of AS 21), Joint venture (defined in terms of AS 27), Associate (defined in terms of AS 23), Promoter-promotee [as provided in the SEBI (Acquisition of Shares and Takeover) Regulations, 1997] for listed companies, a related party (defined in terms of AS 18) Common brand name, and investment in equity shares of 20% and above)."
24. How can a company register as a CIC-ND-SI?
Ans: The application form for CICs-ND-SI available on the Bank's website can be downloaded and filled in and submitted to the Regional Office of the DNBS in whose jurisdiction the Company is registered along with necessary supporting documents mentioned in the application form.
25. A CIC-ND-SI should have 90% investment within the group, and in terms of current exposure norms, NBFCs-ND-SI are permitted only 40% of both lending and investment within any group. Therefore, no NBFC as it stands, would be able to become a CIC without breaching the NOF, CRAR or Concentration Norms, since its entire business is in a subsidiary. However, an NBFC may voluntarily seek to become a CIC-ND-SI since it brings clarity to the holding structure in their organization. How would this issue be resolved? Could NBFCs-ND-SI be provided exemption from Capital adequacy/exposure norms during the transition period, just as unregistered CICs-ND-SI are given 6 months time.
Ans: The NBFC would have to apply to RBI with full details of the plan and exemptions could be considered on a selective basis on the merits of the case.
26. A company has investments in Group companies but does not meet the criteria of principal business as defined in terms of asset-income criteria to be as an NBFC. Can the company still be registered as a CIC or does it need to first register as an NBFC?
Ans: CICs need not meet the principal business criteria for NBFCs.
27. If a company is a CIC but does not exactly meet the criteria specified, does the company need to register as an NBFC?
Ans: A holding company not meeting the criteria for a CIC laid down in para 2 of Notification No DNBS. (PD) 219/CGM(US)-2011 dated January 5, 2011 would require to register as an NBFC. However, if such company wishes to register as CIC-ND-SI/ be exempted as CIC, it would have to apply to RBI with an action plan achievable within the specific period to reorganize its business as CIC. If it is not able to do so, it would need to comply with NBFC requirements and prudential norms.
28. Whether a Holding Company which is not able to comply with the CIC criteria (all four conditions), would still need to comply with NBFC requirements and prudential norms even in the event that it is not satisfying the asset-income criteria. (For example: the holding company owns 60 per cent equity in another group company and is not meeting other three conditions Therefore, it does not qualify as a CIC. Further, the income from financial assets is also less than 50 per cent of total income. Whether such a company would require compliance with NBFC norms).
Ans: No, since the Company is not fulfilling the Principal Business Criteria (asset-income pattern) of an NBFC i.e. more than 50 % of its total assets should be financial assets and the income derived from these assets should be more than 50% of the gross income, it is not required to register as an NBFC under Section 45 IA of the RBI Act, 1934. However it should register itself as an NBFC as soon as it fulfills the criteria of an NBFC and comply with the NBFC norms.
29. A group would like to set up a CIC-ND-SI in the group to rationalize the set up. However, no company can commence the business of NBFI without COR from RBI. Therefore the proposed company would have to apply for COR before transferring shares from different companies to the CIC-ND-SI. But at that time the company would not be eligible in terms of the requirements, as it would not have 90% of net assets as investment in group companies. What should the company do?
Ans: The company would have to apply for COR to RBI, giving a business plan within a prescribed time period of one year in which it would achieve CIC-ND-SI status. In case the company is unable to do so, the exemptions would not apply and the company would have to comply with NBFC capital adequacy and exposure norms.
30. Whether CICs that are exempt from registration either because they have an asset size of less than Rs 100 crore or are not accessing public funds are required to register as NBFCs?
Ans: CICs that (a) have an asset size of less than Rs.100 crore irrespective of whether they are accessing public funds or not and (b) have an asset size of Rs. 100 crore and above and are not accessing public funds have been exempt from registration with the Bank under Section 45IA of the RBI Act, 1934 in terms of notification No. DNBS.PD.221/CGM(US) 2011 dated January 5, 2011. Thus, they are not required to register with the Bank at all. As this is an exemption given under Section 45NC of the RBI Act, 1934, they are not required to approach the Bank at all.
31. Would a similar benefit apply to NBFCs i.e. would NBFCs with an asset size of less than Rs 100 crore and not accessing public funds be exempted from registration with the Bank?
Ans: No, this exemption is specifically given to CICs only. NBFCs other than CICs are not covered by this or any other aspect of the CIC Directions and would have to register with the Bank and comply with all applicable Directions of the Bank as issued from time to time.
32. Should Net assets include operating assets?
Ans: Net assets have been defined in Notification No. DNBS.(PD) 219/CGM(US)-2011 dated January 05, 2011 (para3(1)e) specifically for the purpose of defining a CIC. As such they will only include the items specifically mentioned therein, irrespective of whether any of these qualify as operating assets or not.
33. Definition of Group Companies should include LLPs and Partnerships in the Group?
Ans: Neither LLPs nor Partnerships are companies and hence have been deliberately excluded from the definition of Group Company. Further, in view of the loose structure and regulatory framework for these entities, it is felt that they should not be included in the definition.
34. While instruments that are compulsorily convertible into equity shares within a period not exceeding 10 years from the date of issue are excluded from Outside Liabilities, in terms of the Companies Act such instruments are excluded from the definition of 'public deposit' if they are convertible with a period of 20 years?
Ans: The period of 10 years was specified as a prudential measure not necessarily in alignment with a provision of the Companies Act. Moreover, the issue here is not public deposits but Outside Liabilities.
35. Unlike other NBFCs, can CICs ND-SI (a) no longer make overseas investment or (b) raise ECB or (c) obtain bank finance for acquisition of shares?
Ans: The Directions on CIC-ND-SIs have not restricted them from making overseas investment. Such investment will be governed by the provisions of Chapter VII of Master Direction-Core Investment Companies (Reserve Bank) Directions, 2016. Similarly, presently CIC-ND-SIs can raise funds through ECB. The same would be governed by the instructions contained in the ECB Policy issued by Foreign Exchange Department of the Reserve Bank. Lending to NBFCs/ CICs by banks will be governed by the provisions as applicable to banks and specifically contained in the instructions on 'bank finance to NBFCs' issued by Department of Banking Regulation of the Reserve Bank.
36. If one of the small CICs in a group does not access public funds why should it register based on the condition of aggregate asset size?
Ans: As already clarified in the FAQs, a CIC that does not access public funds is exempt from registration irrespective of having other CICs in the Group that access public funds. Illustratively, if A is a CIC and B and C are also CICs and Group Companies of A provided A does not access any form of public funds including any funds from any Group Company including B and C, it would not require to register as a CIC. If A, B and C do not access public funds in any form none of them would be required to register as a CIC.
37. Will adjusted net worth of all the CICs in the Group also be aggregated for compliance purposes ?
Ans: Adjusted net worth (ANW) is a concept akin to capital requirement wherein the ANW should not be less than 30% of the risk weighted assets (RWA). In cases where asset size is aggregated, all the CICs within the group will be registered as CIC-ND-SI ANW will be applicable individually.
38. There is an apparent anomaly in the definition of 'public funds' as the moment public deposits is included in the definition of 'public funds' and CICs will be deemed to have raised public deposits and will therefore become an NBFC subject to exposure norms?
Ans: Even though public funds include public deposits in the general course, it may be noted that CICs cannot accept public deposits. It may further be reiterated that no NBFC can accept public deposits without specific permission of the Bank even if it holds a CoR from the Bank.
39. Would para 7 of the revised regulatory framework for NBFCs issued vide CC DNBR (PD) CC.No. 002/03.10.001/ 2014-15 dated November 10, 2014 on multiple NBFCs in a group also apply to Core Investment Companies (CICs) in the group?
Ans: No. CICs in a group would not be considered for aggregating the assets of multiple NBFCs in a group under the circular. Instructions contained in the Core Investment Companies (Reserve Bank) Directions, 2011 dated January 5, 2011 shall be applicable to CICs in this regard.
40. What are the asset classification norms applicable to CICs?
Ans: Registered CICs with assets < Rs.500 crore shall follow the asset classification norm as specified in the Non-Systemically Important Non-Banking Financial (Non-Deposit accepting or holding) Companies Prudential Norms (Reserve Bank) Directions, 2015 and those with assets >= Rs.500 crore shall follow the asset classification norm applicable to NBFCs with assets > = Rs. 500 crore as specified in the Systemically Important Non-Banking Financial (Non-Deposit accepting or holding) Companies Prudential Norms (Reserve Bank) Directions, 2015.
41. What are the standard asset provisioning norms applicable to CICs?
Ans: Registered CICs with assets < Rs. 500 crore shall maintain standard asset provisioning of 0.25% as specified in the Non-Systemically Important Non-Banking Financial (Non-Deposit accepting or holding) Companies Prudential Norms (Reserve Bank) Directions, 2015 and those with assets >= Rs.500 crore shall maintain standard asset provisioning of 0.40% which would be applicable as specified in the Systemically Important Non-Banking Financial (Non-Deposit accepting or holding) Companies Prudential Norms (Reserve Bank) Directions, 2015.
42. Are Core Investment Companies (CICs) permitted to invest in Liquid Fund Schemes (Mutual Funds) with maturity of less than 91 days?
Ans:. Yes. As per the present directions for CICs, they are permitted to make investments in money market instruments, including money market mutual funds. Since Liquid Funds are also mutual funds with the underlying being money market instruments; CICs are permitted to invest their surplus funds in Liquid Fund Schemes also.
43. CICs which presently have an asset size of less than Rs. 100 crore are required to apply to the Bank within three months of the date of achieving a balance sheet size of Rs. 100 crore. Would the date of achieving balance sheet size of Rs. 100 crore be the date of the last audited balance sheet ?
Ans: Yes, company which is a CIC and has achieved the balance sheet size of Rs.100 crore as per its last audited annual financial statement is required to apply to the Bank for registration as a CIC-SI, subject to its meeting the other conditions for being identified as systemically important CIC.

redpajama_set_name: RedPajamaCommonCrawl


Today, the ideology of the Caucasus Emirate is a subject of controversy mixed with delusion. Gone are the days of the nationalist guerrilla insurgency which sought to establish an independent Islamic state in Chechnya and Dagestan. Even during the early 1990s, the nationalist banner struggled with radical Salafism propagated from Saudi Arabia, introduced by foreign fighters such as Ibn al Khattab and Abu Umar al-Saif, and then adopted by local jihadist leaders including Shamil Basayev, Anzor Astemirov and later by Said Buryatsky and Doku Umarov. As the 1990s and early 2000s progressed, the rise of Salafist ideology within the Caucasus insurgency became more apparent while secular nationalism was increasingly decaying.
The explicit transformation occurred on October 7, 2007 when leader of the Chechen Republic of Ichkeria (ChRI), Doku Umarov, disbanded the ChRI to establish the Caucasus Emirate, shifting its objective to create an Islamic State based on Sharia law within the entire North Caucasus between the Black and Caspian Seas. However, many security scholars and experts have failed to acknowledge the conversion. It became readily apparent after the terrorist attacks in Boston in April 2013 committed by the Tsarnaev brothers of ethnic-Chechen background, when expert and lay person alike questioned, "Why do Chechens want to attack the United States?" University of Massachusetts Dartmouth's Dr. Brian Glyn Williams, an expert on jihad in Chechnya, who corresponded with Jokhar Tsarnaev via email before the attacks, continues to argue that the Caucasus Emirate is not a Salafist group linked with al Qaeda, but instead that the movement has fallen victim to "years of Russian disinformation, 9/11, and a sloppy American media." Many in the media acknowledge that the Caucasus Emirate is an Islamist radical group but do not make a distinction as to what school of Islamist thought they observe. Some analysts have defined the Caucasus Emirate as Salafist but have not engaged in thorough analysis to present solid evidence based on ideological precepts. This gap between labelling and a wealth of conclusive evidence readily available to those interested on learning about the Caucasus Emirate and the insurgency in the North Caucasus has only led to the confusion and delusion that is spoken of today by experts and the general public. Welcome and beneficial efforts have been made by a few experts on insurgency in the North Caucasus who have correctly identified the metamorphosis of the jihad in the North Caucasus, such as Pavel Baev, Gordon Hahn, Alexander Knysh, Sergey Markedonov and Emil Souleimanov as one that adheres to Salafist-takfiri jihadist ideology.
The aim of this paper is to firmly conclude why the Caucasus Emirate is a Salafist-takfiri jihadist terrorist group by analyzing speeches made by the leaders of the Caucasus Emirate and the messages promoted on their many websites and internet-based propaganda platforms. Their rhetoric will be matched with the core tenets of this ideology. Furthermore, this paper will underline why the Caucasus Emirate has long been a threat to international security interests and will continue to be so for the foreseeable future.


text:
The Tripod Complex Fire was a wildfire which burned in north-central Washington state in 2006. The complex consisted of two wildfire complexes which later merged into a single fire: the Spur Peak Fire and the Tripod Fire. Both were caused by lightning strikes. The Tripod Complex burned a total area of , making it one of the largest wildfires in Washington history at the time.

Events

Prolonged hot and dry weather, combined with an outbreak of mountain pine beetles and a large number of thunderstorms made the 2006 wildfire season of the most severe in Washington state history. The 2006 Pacific Northwest wildfire season began in late June, when an extended thunderstorm followed a three-day heat wave. Between June 27 and July 10, lightning strikes occurred almost daily.

Lightning ignited several wildfires during this period—including the Spur Peak Fire, which was first reported on July 3. Located in the Okanogan National Forest, the fire was deemed fully contained by July 14.

A second thunderstorm in late July set off another round of wildfire activity in the region. On July 24, a new fire burning just south of the Spur Peak Fire was reported: the Tripod Fire. Smokejumpers from the North Cascades Smokejumpers base in nearby Winthrop, Washington— from the point of ignition—were quickly dispatched to the fire. Despite early containment efforts, low humidity and gusty winds allowed the Tripod Fire to grow rapidly. The extreme fire weather also re-intensified the previously contained Spur Peak Fire, which crossed control lines on July 27. The two fires converged in late August.

In mid-August, a battalion of 550 United States Army soldiers were deployed to fight the Tripod Complex Fire. It was the first time a military battalion had been used to fight a wildfire in the US since 2003. By August 23, the Tripod Complex had grown to  and around 3,000 firefighters were assigned to the fires. Washington governor Christine Gregoire surveyed the complex by helicopter and later declared a statewide wildfire emergency, stating "numerous wildfires across Washington pose a serious threat to homes, infrastructure, businesses and natural resources".

The Tripod Complex was extinguished in October, when snowfall ended the wildfire season. The complex had burned a total of .

References

2006 in Washington (state)
2006 wildfires in the United States
Okanogan County, Washington
Okanogan National Forest
Wildfires in Washington (state)

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}

Since the discovery nearly 25 years ago of the SiO molecule in Orion
(Snyder \& Buhl 1974), SiO masers have
been observed in the envelopes of hundreds of late-type stars, and in the
direction of a few
galactic HII regions. Orion remains a unique source of SiO emission
because it contains all known SiO isotopic species and because it is
the only star-forming region exhibiting a very strong maser in the
$v=1, J=2 \rightarrow 1$ transition. The strong and
compact $v=1$ SiO maser is associated with the luminous infrared
source IRc2 and is closely connected with the extended and weaker
$v=0$ maser emission mapped at 43 GHz (Chandler \& De Pree 1995) and 86
GHz (Wright et al. 1995).
Recent high resolution observations showed that IRc2 is a complex
object resolved into
four components (Dougados et al. 1993) and that the center of the
strong ($v=1$) and weak ($v=0$) SiO
maser outflows coincide with the radio continuum source I
(Menten \& Reid 1995, Wright et al. 1995), and is displaced from the
center of the molecular hot core (lying to the east of source I). On
the other hand, the center of the large-scale high velocity bipolar
outflow traced by CO lies roughly $3"$ to the north of
source I.

 Considerable efforts have been made to properly model the SiO maser
phenomenon in late-type stars. Models include radiative and/or collisional
excitation
schemes (e.g. Kwan \& Scoville 1974, Elitzur 1980,
Langer \& Watson 1984, Lockett \& Elitzur 1992 or Bujarrabal 1994). All
models share
two general characteristics:
$(i)$ they require high volumic densities of order
$10^{8}-10^{10}$ cm$^{-3}$; $(ii)$ inversion of the SiO level populations
depends on the column
density, and maser emission in higher vibrational states peaks at
higher values of the column density. On the
other hand, there are major observational facts that cannot be explained
by any of the present radiative/collisional SiO pumping schemes. In
particular, the "standard" pumping schemes fail to explain in stars
the peculiar distribution of line intensities within a given
vibrational state (e.g. Cernicharo \& Bujarrabal 1993), and fail to
explain the absence or weakness of $v=2, J=2 \rightarrow 1$ emission
from Orion and late-type stars (Olofsson et al. 1981 b, Bujarrabal
et al. 1996). In fact, line
overlaps among transitions of the isotopic species of silicon
monoxide are an important addition to radiative/collisional
pumping in stars (e.g. Gonz\'alez-Alfonso \& Cernicharo 1997), while
the line overlap between two near infrared lines of SiO and water
explains the weakness of the $v=2, J=2 \rightarrow 1$ transition
(Bujarrabal et al. 1996).

 Depending on the relative importance of property $(ii)$ above (namely
various $v$ state masers should peak in different spatial regions)
with respect to line overlap effects among nearby transitions of
SiO and isotopes the spatial distribution of various vibrational transitions
should differ or not. Therefore, high spatial resolution and sensitive
maps of SiO and isotopes should provide a test of these predictions.
With this idea in mind we have
compared the spatial distributions of two nearby transitions of
\dSiO and \uSiO toward Orion IRc2 which
contains the strongest SiO source in the sky. In Sect. 2 we
present our observations and give details of data reduction. In Sect. 3
we discuss spectral variability and present our maps of \dSiO and \uSiO
emission
from Orion. In Sect.~4 we discuss some properties of the apparent ring of
\dSiO and
\uSiO masers, the relative spatial extents of both
species and implications on their excitation. Some conclusions are
summarized in Sect. 5.

\section{Observations and data reduction}
In order to compare the relative spatial distributions of the main
(\uSiO) and rare
isotope (\dSiO) emissions we need a relative positional accuracy
better than the extent of the main isotope emission, $\approx 0.15"$.
For this kind of accuracy simultaneous observations
of two different transitions are appropriate. We thus searched for nearby
frequencies
involving rotational levels not too high in energy.
The frequencies of the $v=0, J=2 \rightarrow 1$ and $v=1, J=2 \rightarrow 1$
transitions of \dSiO and \uSiO (85.75913 and 86.24337 GHz) differ by less
than the 500 MHz instantaneous bandwidth of the
interferometer and can thus be simultaneously observed.
Observations of these two lines in Orion IRc2 were made on
August 19 and 21, 1995 and March 5, 1996 with four antennas of the IRAM array
on Plateau de Bure (see Guilloteau et al. 1992 for details) . In 1995 we used
configuration B2 with antennas on stations N17 E24 W09 W12 and spacings
covering 24 to 288 m. The synthesized beam was around $3.5" \times 1.4"$.
Higher spatial resolution was achieved in 1996 with
antennas on stations N29 E24 W20 W27 corresponding to spacings from 56 to
408 m and resulting in  $2.6" \times 1"$ resolution.
The independent correlator units of the interferometer were used as
follows. The $v=0,
J=2 \rightarrow 1$ and $v=1, J=2 \rightarrow 1$ lines of \dSiO and \uSiO
were placed in two 20 MHz sub-bands
centered at 113.75 MHz and 596.25 MHz, respectively.
The frequency separation between adjacent spectral channels was
78.1~kHz, or  0.27 km s$^{-1}$.
In 1995, for
redundancy, the
\dSiO $v=0$ line was also observed in a 40 MHz wide sub-band.
Broad band
continuum observations with three or two 160 MHz units were performed
simultaneously.
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure1.epsf}
  \end{center}
\caption[]{Cross-correlation spectrum of the $v=0, J=2 \rightarrow
1$ line of \dSiO observed with the
IRAM array on 1995 August (continuous line) and 1996 March (dotted line).
The separation between channels was
0.27 km s$^{-1}$. 1 K corresponds to a flux density of 24 Jy.}
\label{variable29SiO}
\end{figure}

 In this project we have mapped the \dSiO and \uSiO line emissions using
one of the strongest features of the main isotopic species to
self-calibrate all
data. Therefore, a careful bandpass calibration was required across the entire
bandwidth since the maximum frequency separation between extreme
features of both species is around 496 MHz. To this end we observed
strong calibrators, 3C454.3, 3C273, $0528+134$ or $0415+379$. In
1995 our best results were obtained  with
3C454.3 which we observed just before a long run in Orion. Although we do not
expect a priori any short time-scale variations of the bandpass shape, we
used a
different scheme in 1996. Observations of Orion were interspersed with
those of the bandpass calibrator $0415+379$.
Nearby phase calibrators were not essential for this project since we
self-calibrate the data on one of the main spectral features. The
bandpass calibrators were used to calibrate the flux density scale. At 86
GHz we adopted
6.5 and 10 Jy for 3C454.3 (1995 August observations) and $0415+379$
(1996 March observations), respectively. Although the flux density for
$0415+379$ was uncertain because it was highly time variable in 1995
and 1996, we averaged our measurements of the antenna temperature to Jy
conversion
factor for both observing periods and adopted S/T = 24 Jy/K.

 Data reduction was performed with the CLIC package (Lucas 1996). The sky was
clear during the observations and little editing was necessary. However,
we discarded some of the 1995 data when Orion was too low on the horizon.
The bandpass solutions
were determined by fitting the complex gains in several sub-bands ; these
solutions
were applied to the line data base. In 1995 each day
was treated separately.
\scriptsize
\begin{table} [t]
 \hspace* {-1. cm}{ {\scriptsize{
 \caption{Signal to noise ratio and errors for
 observations of 1996 March (the synthesized beam is of order 1.6").}
\begin{tabular}{l c c c}   \hline
      {\bf SNR and Error} & {\bf \uSiO}  & {\bf \dSiO} & {\bf \dSiO/ \uSiO}
\\ \hline\hline
      {\em SNR} & 200-25000 & 150-400 & 150-25000 \\
      {\em r.m.s. phase (degree)$^{1}$} & 0.002-0.29 &
      0.14-0.38 &
      0.14-0.48\\
      {\em r.m.s. position (mas)}  & 0.03-4 & 2.0-5.3 & 2.0-6.6 \\
\hline
{\em bandpass phase (degree)$^{2}$} & 1 & 1 & \\ \hline
{\em phase shift (degree)$^{3}$} & & & 1 \\
{\em position shift (mas)} & & & 4.4 \\ \hline
\end{tabular}}}}
 $^{1}$Phase noise due to finite signal to noise ratio; the
corresponding position error is ${\sigma}_{\phi}\simeq 0.5\times
1.6"/SNR$. \\
 $^{2}$Typical total bandpass phase noise; the channel to channel IF
noise is
negligible and less than 0.1 degree. \\
 $^{3}$Maximum phase shift between \uSiO and \dSiO sub-bands; one degree
phase shift corresponds to 4.4 mas with 1.6" synthesized beam.
\end{table}
\label{erreur}
\normalsize
To improve the phase stability
we determined accurate baseline solutions and we applied the known
antenna axis corrections. The phase residuals lied in the range $4
\rightarrow 30$ and $4 \rightarrow 8$ degrees for the 1995 and 1996
observations, respectively.
We then mapped the \uSiO
and \dSiO line emissions using the task UV\_ASCAL and one strong feature of
the main
isotope to self-calibrate all other features. Accordingly, we are
insensitive to atmospheric phase fluctuations and to any systematic errors
left in the baseline calibration. The position accuracy within the \uSiO
and \dSiO spot maps is limited by
finite signal to noise ratio and by imperfect bandpass calibration
(see Table 1).
In practice, the position errors within our \uSiO maps lie around
$1-2$ milliarc sec (mas) in RA and $4-5$ mas in Declination. This
allows us to discuss the long-term stability of the velocity pattern
observed for both isotopes, as well as the long-term
stability of the \uSiO emission ring discussed in Sect. 4.1.
When one compares the relative positions of the
\dSiO and \uSiO emissions, the relative phase shift of the two \uSiO
and \dSiO sub-bands cannot be neglected (Table 1); we found a maximum
drift of 1 degree per hour for the March 1996 observations. Because
we regularly calibrated the bandpass in 1996, the position error
between both isotopic species due to phase shift between sub-bands was
less than 5 mas. This error is estimated to be about
ten times higher in our data of 1995 August due to much less time
spent in bandpass calibration. In Sect. 4.4, we only discuss the
relative positions of both isotopic species observed in 1996. The
overall relative \uSiO to \dSiO position uncertainty is of order 5-8 mas.

\section{Results}

\subsection{\dSiO $v=0, J=2 \rightarrow 1$ emission}
 The \dSiO v=0 line at 85.759 GHz was
discovered in Orion by Olofsson et al. (1981 a) who observed
narrow and time variable features. The
maser nature of this emission is well demonstrated here because we detect
narrow spectral emission of same intensity with all baselines of the
array. \dSiO $v=0$ emission will be discussed further in Sect. 4.2 and
is essentially unresolved with the IRAM connected array (see below, however).
In addition, we
observe spectral variability over the 6.5 months period of our two observing
sessions since both the line shape and relative peak intensities clearly
changed with time (Fig. \ref{variable29SiO}).
The emission spectrum consists of two main features in the
velocity range $-11 \rightarrow 0$ and $10 \rightarrow 24$ km s$^{-1}$.
This is similar to the \uSiO emission range although
\dSiO and \uSiO emission profiles are much different, a fact which
can partly be related to differences in the degree of saturation of
both masers. There is weak emission in the intermediate velocity range
$0 \rightarrow 10$ km s$^{-1}$. This
\dSiO emission is about 20 times weaker than in \uSiO, and is
detected with all baselines of the array.
However, with the 24-m long baseline available in 1995,
the \dSiO emission lying between the two
main features was nearly 5 times stronger than for all other longer
baselines. We conclude that for this baseline there was a blend of
quasi-thermal and maser \dSiO emission. Both maser emission and quasi-thermal
emission were also observed in the $v=0$ state of the more abundant
species \uSiO (Chandler \& De Pree 1995, and Wright et al. 1995 for
the $J=1-0$ and $J=2-1$ transitions, respectively). Wright et al.
showed that the \uSiO $v=0$ maser component extends over $\approx 2"$
although it is closely connected with the $v=1, J=2-1$
compact masers. On the other hand, their \uSiO
$v=0$ low spatial resolution maps are more sensitive to thermal
emission and show a connection with the high
velocity bipolar CO outflow ($\approx 25" \times 45"$ in size).
For all \dSiO spectra and data discussed in
this work we restricted the analysis to $(u,v)$ distances
greater than about 50 m and 25 m for our observations of
1996 March and 1995 August, respectively. We were thus insensitive to
structures extending over $\approx 10" - 30"$.

 Fig. \ref{29SiOrelatmap} shows the relative positions of \dSiO $v=0, J=2
\rightarrow 1$ maser spots observed in 1996.
We used the strong \uSiO $v=1, J=2 \rightarrow 1$ maser feature
at 15.6 km s$^{-1}$ to self-calibrate these data (cf. Sect. 2),
and we verified that selection of a specific reference feature
was not critical. The \dSiO $v=0$ emission is distributed
along two ridges of positive and negative velocities as for \uSiO
(compare Fig. \ref{29SiOrelatmap} with Figs. \ref{relat28map}
and \ref{relat28mapbis}) with stronger \dSiO $v=0$ features
excited at the edge of each ridge contrary to \uSiO. The
mean distance between the two \dSiO ridges is of order $0.13"-0.14"$.
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure3.epsf}
  \end{center}
\caption[]{Spot map of \dSiO $v=0, J=2 \rightarrow 1$ emission observed on 1996
March. The small open squares correspond to the centroid of emission in one
spectral channel. Each channel is
separated by 0.27 km s$^{-1}$. The center of the brighter channels is
surrounded by a circle whose diameter is proportional to the peak
intensity in these channels. The LSR velocities are shown for the
brighter channels, and, for clarity, the circles and velocity labels are given
every 6 channels.}
\label{29SiOrelatmap}
\end{figure}
This picture is fully consistent with our 1995 results
although the mean distance
between the two ridges was slightly narrower in 1995 and of order $0.11"$.
The 20
to 30 mas change between the two ridges observed in 1995 and
1996 seems real because it is greater than the typical relative position
error of the
individual \dSiO features.
At both epochs of observations the data were acquired
with non rotating antenna feeds sensitive to
vertical polarization only. However, we are not affected by polarization
effects
because we have verified that our relative spot maps
were nearly identical when we analyzed the data over short periods
with a small range of paralactic angle.
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=15.cm
     \epsfbox{figure4.epsf}
  \end{center}
\caption[]{Cross-correlation spectrum of \uSiO $v=1, J=2 \rightarrow 1$
emission observed on 1995 August (continuous line) and 1996 March (dotted
line). The upper panel shows the overall spectrum and the lower panel
shows the weak features around 23 to 33 km
s$^{-1}$ and intermediate velocity emission around $4 \rightarrow 10$ km
s$^{-1}$. The separation between individual channels
is 0.27 km s$^{-1}$. 1 K corresponds to a flux density of 24 Jy.}
\label{weak28SiO}
\end{figure}
\subsection{\uSiO $v=1, J=2 \rightarrow 1$ emission}
The \uSiO $v=1, J=2 \rightarrow 1$ spectrum is dominated by two
strong, time variable
features lying around $-2 \rightarrow -10$ and $12 \rightarrow 20$ km
s$^{-1}$. In addition, the line profile exhibits weak
features around 30 km s$^{-1}$ which were first detected by Wright et
al. (1995; see their Fig. 1). These features are present in our 1995
and 1996 data
(Fig. \ref{weak28SiO}). Comparison with the line
profile obtained by Wright et al. with similar spectral resolution shows
that they are time variable. The peak flux around 30 km s$^{-1}$ is
around 18 Jy in Wright et al. while we measured 10 Jy in March 1996.
Variability and detectability with all six
baselines of the array suggest that these weak features are masing as
the bulk of the \uSiO emission; see, however, discussion in Sect. 4.2.
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure5vit.epsf}
  \end{center}
\caption[]{Spot map of \uSiO $v=1, J=2 \rightarrow 1$ emission observed
on August 19, 1995. Each velocity channel is
connected and, for clarity, the LSR velocity labels are given every 5
channels. The velocity separation between each open square is 0.27 km
s$^{-1}$.}
\label{relat28map}
\end{figure}
Our map of relative positions of $v=1, J=2 \rightarrow 1$ maser
emission observed in 1995 August is
shown in Fig. \ref{relat28map}; in Fig. \ref{relat28mapbis}
we also show the relative intensities of the main features. The
position$-$velocity pattern present in Fig. \ref{relat28map} or
\ref{relat28mapbis} is consistent with our 1996 observations (open
squares and small full circles in Fig. \ref{relat2829map}) and with
that observed in 1995 January by Wright et al. (1995).
All maps show similarities.
There are, however, minor but obvious changes among the different
maps including changes for the weak high velocity features which seem to
have moved during the period 1995 January to 1995 August and 1996 March.
On the other hand, the mean distance between the main negative and positive
velocity features remains stable. For our 1996 observations we
measured a separation of 0.16", a value very close
to that deduced from our 1995 results
and earlier IRAM results, and consistent with the BIMA array results
(see discussion in Sect. 4.1).
The absolute position of the \uSiO maser was measured by
Wright et al. (1990) and Baudry et al. (1995) to an accuracy of $\approx
0.15"-0.20$".
Menten \& Reid (1995) found that the centroid  of the SiO maser
distribution coincides with the radio continuum
source, I, lying on the southern edge of the complex source IRc2.
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure5rond.epsf}
  \end{center}
  \caption[]{Spot map of \uSiO $v=1, J=2 \rightarrow 1$ emission observed
  on August 19, 1995. Each small open square marks the center of an
  individual channel whose velocity is given in Figure \ref{relat28map}.
 The diameter of each circle, given every 3
  channels, is proportional to the line intensity.}
  \label{relat28mapbis}
\end{figure}
\section{Discussion}
\subsection{Stability of the ring of \uSiO masers}
The regular position$-$velocity pattern of $v=1, J=2 \rightarrow 1$
emission (Plambeck et al. 1990, Wright et al. 1995) was interpreted
by Plambeck et al. as a collection of
maser clumps lying in an expanding and rotating disk. This pattern
does not change much with time
and has been observed with the IRAM interferometer in 1990
(Guilloteau et al. 1992), 1992 (Baudry et al. 1995), and 1995 and
1996 (this work).
A similar position$-$velocity pattern was also observed in the $J=1
\rightarrow 0$
transition of SiO around 43 GHz by Morita et al. (1992) and Menten \& Reid
(1995).
We can estimate the long-term
stability of the 86 GHz pattern by measuring the mean separation
between the two ridges delineated by the
dominant positive and negative velocity features of
Orion IRc2. To this end, we have used the 6 different maps
made at 86 GHz with the BIMA and IRAM
interferometers (Plambeck et al. 1990, Wright et al. 1995, Guilloteau
et al. 1992, Baudry et al. 1995, and this work). The general
orientation and the mean separation between the two ridges of main SiO
features do not seem to evolve with time.
The mean separation between these two ridges is $\approx 0.^{''}165 \pm
0.^{''}01$;
for the uncertainty we have assumed that the 6 independent measurements
behaved as gaussian variables. Therefore, any apparent contraction or
expansion
of the ring, would be less than or of order $0.^{''}01 / 7$yr, namely
$\leq 0.7$ AU/yr at the 480 pc distance of Orion A. On the other
hand, stability of the
intermediate velocity pattern ($\approx 0 \rightarrow 11$ km s$^{-1}$)
is not obvious when we compare our 1990 data with the present IRAM
maps. The complex shape observed in 1995 or 1996 is not quite similar to
that in 1990 (see
Fig. 11 in Guilloteau et al. 1992). Such differences cannot be due to
relative position errors which are less than about 2 to 5 mas in the
\uSiO maps. These discrepancies seem
to agree with the model of Plambeck et al. (1990) which
predicts that intensity changes in the intermediate velocity features
could cause large position changes of the maser spots in the disk.

\subsection{Nature of the \uSiO high velocity features}

 The high velocity features lying around $28\rightarrow 31$ km s$^{-1}$ are
located
close to the positive
velocities of the SiO ring (see e.g. the 29.2 and 29.1 km s$^{-1}$
features in Figs. \ref{relat28map} and \ref{relat2829map}).
Our observations of 1995 August show that these features are excited in an
area similar,
although not identical, to that observed in 1995 January by Wright et al.
(1995, see their Fig. 1c)
for their $30 \rightarrow 33$ km s$^{-1}$ features.
However, 6.5 months later our data show that the $28 \rightarrow
31$ km s$^{-1}$ features have migrated toward the
most positive velocity end of the main SiO emission ridge
(see location of the 29.1 km s$^{-1}$ component in Fig.\ref{relat2829map}).
The apparent migration of weak high velocity components is consistent
with the model of Plambeck et al. (1990) where small changes in
brightness distribution of extended features may look like rapid motion.
Nevertheless, such rapid motions should be confirmed in future maps
of \uSiO emission. These high velocity
features could be related to the spectral changes observed for the
same components; they could be weakly masing as suggested in Sect.
3.2. It is interesting to note that anomalous gas motion beyond
the expansion velocity of the ring of maser
clumps could perhaps explain the high velocity components. Such components
are reminiscent of the weak features observed in the line wings of
\uSiO emission from late type stars (Cernicharo et al. 1997, Herpin et
al. 1998). SiO line wing emission in stars is related to bipolar gas
outflows and
to pulsations of the underlying star.
\begin{figure} [t]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure6vit.epsf}
  \end{center}
\caption[]{Comparison of \uSiO $v=1, J=2 \rightarrow 1$ and \dSiO $v=0, J=2
\rightarrow
1$ spot maps using the \uSiO feature at 15.6 km s$^{-1}$ as a phase
reference in both maps. The epoch of
the observations was March 5, 1996 for both isotopes. We have plotted the
centroids of the \uSiO features (open squares and small full circles)
together with the main \dSiO features (dotted circles). The diameter of
each circle is
proportional to the peak intensity for \dSiO. The LSR velocity labels
are given every 5 and 6 channels for \uSiO and \dSiO, respectively.}
\label{relat2829map}
\end{figure}
\begin{figure} [tbh]
  \begin{center}
     \epsfxsize=8.5cm
     \epsfbox{figure6rond.epsf}
  \end{center}
\caption[]{Comparison of \uSiO $v=1, J=2 \rightarrow 1$ and \dSiO $v=0, J=2
\rightarrow
1$ spot maps using the \uSiO feature at 15.6 km s$^{-1}$ as a phase
reference in both maps. The epoch of
the observations was March 5, 1996 for both isotopes. We only show the
centroids of
\dSiO (dotted circles) and
\uSiO (full circles) emissions. The diameter of each circle is
proportional to the peak intensity.}
\label{relat2829mapbis}
\end{figure}
\subsection{Nature of the \dSiO $v=0$ emission}
Time variability as well as notable changes in the \dSiO line profile
(Fig.
\ref{variable29SiO}) are clearly in favour of maser emission.
Short-term variability
in the excitation of the \dSiO molecule is suggested by
our maps because the mean distance observed in
1996 between the two ridges of emission, $\approx 0.13"-0.14"$, is
significantly
larger than the $0.11"$ measured in 1995. This fact indicates non
thermal processes in the excitation of \dSiO. In addition, the relatively
high flux density
observed in 1995 and 1996 suggests also non thermal emission. The
array cannot give the size of the individual features, but we may use the
synthesized beamwidth and the observed peak flux density to estimate a
minimum brightness temperature. In March 1996 the flux density peaks
around 37 Jy and we derive $T_{B} \geq 2500$ K. This temperature is greatly
above the
kinetic temperature usually adopted in Orion, $\approx 60$ K, and is
another indication
for maser emission although high temperatures would be plausible in a
shocked environment. However, for some of the weaker \dSiO features
in the range $0\rightarrow 10$ km\thinspace s$^{-1}$ we obtain T$_{B}\geq 80-100$ K,
and \dSiO could thus be part thermal and part maser.

 The actual spatial structure of the \dSiO $v=0$ emission is complex,
and we recall that Fig. \ref{29SiOrelatmap} does not show all of the
emission detectable with the array. By discarding the shorter baselines (Sect.
3.1), we have concentrated our analysis on more
compact emission sources. We were not able here to
map the \dSiO $v=0$ emission counterpart to the extended \uSiO $v=0$ emission
seen by Wright et al. (1995).

\subsection{Comparison of the \dSiO and \uSiO spot maps. Implication
on excitation mechanisms}
The relative distribution of \uSiO and \dSiO emission observed in 1996
is shown in Fig. \ref{relat2829map} and in Fig. \ref{relat2829mapbis}
where, for clarity, we have not given the velocities. The two ridges of
\dSiO $v=0, J=2
\rightarrow 1$ emission (dotted circles) and \uSiO $v=1, J=2
\rightarrow 1$ emission (full circles) are clearly visible on these
figures. Our data do not show
a complete spatial overlap as well as a close correlation among features of
both species although in both cases the positive velocities lie to the NW
of the negative features. Another clear difference between \dSiO and \uSiO
is that there is
no obvious pattern for the \dSiO intermediate velocity features (Fig.
\ref{29SiOrelatmap} or Fig. \ref{relat2829map}); this could be
related to mixed thermal and masing features as suggested in the
previous Section.

 Fig. \ref{relat2829map} shows that velocities in the range $ \approx
-6 \rightarrow -10$ km s$^{-1}$ tend to be found in the same area for both
species although it is not possible to make an exact position-velocity
pairing of
the \dSiO and \uSiO features. In Fig.
\ref{relat2829mapbis} the northern ridges of both \dSiO and \uSiO
seem to be co-aligned and are not coincident. We cannot exclude, however,
that uncorrected instrumental effects still affect our relative map and these
observations should be repeated using frequent bandpass calibrations as
used in 1996. In order to force the spatial coincidence
of the main features in both species we have shifted the main \dSiO
features lying around 16 km s$^{-1}$ on top of
the \uSiO features in the range $15 \rightarrow 17$ km s$^{-1}$. Nevertheless,
the \dSiO negative velocity emission
ridge appears well outside the \uSiO negative velocity ridge. Any rotation of
coordinates axis around the 16 km s$^{-1}$ features does not improve the
spatial coincidence of both species. Hence, we conclude that both isotopic
species
are not excited in the same gas layers. This is strengthened by the analysis
of our 1995 data which similarly show no spatial coincidence and a smaller
distance between the two ridges of emission for \dSiO than for \uSiO .

 We note that a similar picture also emerges from the 43 GHz
interferometric observations made by Morita et al. (1992) in Orion.
Although their observations of the \uSiO $v=2, J=1 \rightarrow 0$ and $v=1, J=1
\rightarrow 0$ transitions were not made simultaneously and were less
sensitive than here,
the mean separation between the two ridges of emission is slightly smaller for
$v=2$ ($\approx 0.12"$) than for $v=1$ ($\approx 0.14"$ in agreement
with the separation measured on the 43 GHz map of Menten \& Reid 1995).
The 43 GHz observations, the maps of \uSiO $v=1$ and $v=0$
emission (Wright et al. 1995) and our 86 GHz maps indicate that
different vibrational states of silicon monoxide do show a close connection
but do not exactly coincide.

 We comment below on possible explanations of the observed
similarities without exact co-location of \dSiO ($v=0$) and
\uSiO ($v=1$) maser sources. First, the silicon
monoxide reservoir seems identical for both isotopic species since
their large-scale spatial distributions are alike. This
is expected if shocks generated in the expanding flow traced by the
$v=1, J=2 \rightarrow 1$ masers enhance the sputtering of silicon
which will then react quickly in the gas phase to form both \dSiO and
\uSiO. Second, differences in the small-scale spatial distributions of
\dSiO and \uSiO could simply result from differences in the excitation
of both species or from different physical
conditions within the silicon monoxide cloud. SiO pumping models
do not require any isotopic differentiation to obtain \uSiO, \dSiO or
$^{30}$SiO maser sources. In all cases the general physical conditions
are grossly similar for one isotopic species or another apart from the
total column densities.
On the other hand, all radiative/collisional pumping models show that
different $v$ state masers peak in different spatial regions.
We believe that this fact, combined with different
degrees of saturation in the \uSiO and \dSiO masers, is essential
to explain the slightly different distribution of \dSiO ($v=0$) and
\uSiO ($v=1$) maser spots. Our maps
of relative \uSiO and \dSiO emission also show that some features from
both isotopes and with different velocities tend to be excited in
the same area. This is observed in the range $-6 \rightarrow -10$ km s$^{-1}$.
Collisional pumping
with high temperature ($\approx 1500$ K) and high molecular hydrogen density
($\approx 10^{9}-10^{10}$ cm$^{-3}$) provides
a range of \uSiO column densities where both $v=1$
and $v=2$, $J=1 \rightarrow 0$ masers are excited (Lockett \& Elitzur
1992). Such a
scheme does not apply to our apparently overlapping \dSiO ($v=0$) and \uSiO
($v=1$) 86 GHz features because their velocities are not in good agreement.
However, further observations should be conducted to investigate
the detailed kinematics and stability of the \dSiO emission.

 Line overlap effects among
various transitions of silicon monoxide cannot be ignored to explain
the excitation of this molecule.
First, {\em local} line overlaps due to turbulence play a role
as soon as the velocity dispersion reaches about 5 km\thinspace s$^{-1}$.
Limiting ourselves to the lower $J$ values, we find that 10 to 15
ro-vibrational transitions of \uSiO, \dSiO and \tSiO overlap within 5
km\thinspace s$^{-1}$ for $\Delta v=2$ and 1. If local line overlaps would dominate the
excitation of low $J$ rotational levels in Orion, we would expect
exact spatial coincidence of the isotopic species. Our \dSiO and
\uSiO maps contradict this idea. Second, {\em non-local}
line overlap effects as described by
Gonz\'{a}lez-Alfonso \& Cernicharo (1997) in a non static
circumstellar environment are most important. The relative
distribution of \uSiO and \dSiO emission in our maps is not
inconsistent with such non-local line overlaps. In addition, it is also
plausible
that the overlap between two near infrared lines of water
and \uSiO (Olofsson et al. 1981 b) is an
important excitation process of silicon monoxide in Orion.

 Analysing the spatial extents of different $v$ state masers is clearly
important to better understand the pumping mechanisms of the SiO molecule.
This kind of work should be extended to strong stellar
SiO-emitters since the physical conditions in late-type stars and
Orion are so different. VLBI observations are required in stars in order
to make a detailed comparison of the different $v$ emission layers;
such observations have been made for the first time to map
the $v=2, v=1, J=1 \rightarrow 0$ lines in W Hya and VY CMa (Miyoshi et al.
1994).

\section{Summary}

We have made the first spot map of \dSiO $v=0, J=2\rightarrow 1$
emission from Orion, and we confirm its maser nature. However, there
is also a blend of thermal emission with maser emission.
The \dSiO $v=0, J=2\rightarrow 1$ stronger emission is
distributed along two ridges of positive and negative velocities as
for the \uSiO $v=1, J=2\rightarrow 1$ transition. The spatial extent is
similar but
not identical for the $v=0$ and
$v=1$ masers in agreement with model calculations which predict
that various $v$ state masers peak in different spatial
regions. For those apparently overlapping $v=0$ and 1
features the differences observed in the velocities suggest also that
\dSiO and \uSiO lie in different $v=0$ and 1 gas layers. Turbulence
and high gas temperature implying local line overlap effects
among transitions of \dSiO and \uSiO are unlikely to play a major role
in Orion. However, overlaps among Doppler-shifted ro-vibrational lines
are not excluded.

 We have discussed the long-term stability of
the \uSiO $v=1, J=2 \rightarrow 1$ emission
disk; relative motion between the two ridges of main emission
is less than $\approx 0.7$ AU/yr. We
confirm the detection of features at velocities as high as
about 30 km s$^{-1}$; they could be either rapidly moving weak masers
or extended features with changing brightness distribution.

\acknowledgements
{This work was supported by the CNRS URA 352. We thank the IRAM
staff on Plateau de Bure for their efficient help during the
observations, and we thank M.C.H. Wright for his useful comments.}

redpajama_set_name: RedPajamaArXiv


Pair of reusable nail art gem clusters, curved back to fit the surface of the nail.
Application: Apply a few drops of nail glue on finished nail and place in the desired location, hold for several seconds until secure.
Modifying spinners is not advised as this can place the spinner under undue stress. Modifying the spinners will invalidate the returns policy for this item.