IT'S EASY TO MAKE A PAYMENT TO RESERVE YOUR HUNT or simply pay the balance. If you wish to pay by credit card, please click the 'BuyNow' button below. You will be charged a 3.25% convenience fee on all credit card payments. We welcome your personal or business checks without a convenience fee.
BEFORE YOU CLICK THE BUY NOW BUTTON: Make sure you know the cost of your hunting package before you click. If making a 50% deposit, enter that amount when you hit the button. IF YOU ARE MAKING A PAYMENT FROM AN INVOICE – put the amount of the payment in the next window after you hit the BUY NOW button.
Hunting price list terms and conditions: All prices are subject to change. Price and hunting dates are confirmed with invoice once 50% of the hunt price is received. Payments are non-refundable but can be applied toward another hunt based on availability. Every effort will be made to accommodate you. Final balance of each hunt is due and payable -30- days prior to arrival.
We are an honest, hard working outfit, but make no guarantees related to hunt success! We have no control over adverse weather conditions such as heavy rain, snow, heat and drought, floods or wildfires that Mother Nature may impose on us! Nor do we have any control over a hunter's physical conditioning or shooting abilities! However, we do guarantee to do everything within our control to see that our guests have a safe, successful, and memorable experience while hunting with All American Outfitter! We believe that hunting success is a great reward for good planning, reasonable preparation and serious efforts by all involved! A little bit of "Lady Luck" doesn't hurt anything either!
We suggest each hunter recognize the importance of proper physical conditioning for his or her chosen hunt and get in the best shape possible. Also, know your weapon. Make sure it is properly sighted in and practice shooting from different yardages and positions. The hunter that is prepared physically and knows his weapon well will generally have a more enjoyable and successful experience, and it could mean the difference between a once-in-a-lifetime trophy or a terrible disappointment. As a final note, we suggest that our hunters come mentally prepared with a good sportsmanlike attitude and a sincere desire to hunt. And remember, the success of a hunt shouldn't be measured by the size of a trophy head alone, but rather by the total experience.
EFFECTIVE MAY 15, 2014: Once your hunt is booked with a deposit and for any reason you need to reschedule or postpone your hunt, there will be a 20% fee added to the price of the entire hunt for rescheduling (based on our ability to reschedule and on availability).
Click here to purchase your license online including your Sandhill Crane stamp.
RESERVE A DATE: 50% of the hunting package price is required to reserve date with the balance due 30 days prior to your arrival at AAO. Deposits are non refundable. Cash, check or credit card (through PayPal) is acceptable payment for your hunting packages. We cheerfully accept credit cards via PayPal. There is a 3% convenience fee added to any credit card payment as shipping-handling for using a credit card. If you send a check, there are NO additional shipping-handling fees. If you DO NOT have to have a PayPal account to pay with a credit card – simply scroll down in the payment window and click on 'I don't have a PayPal account" and you will be directed to the credit card window.
ARRIVAL TIME: Hunters will arrive AFTER 3:00PM CST but by 6:30PM on the date of scheduled arrival. Departure time will be clearly stated on your hunting invoice. If you arrive PRIOR TO or need an additional overnight stay and it is not available at AAO, you will need to secure lodging at your own expense. Arrival and departure dates and time are firm at the time of booking and can only be altered at the outfitters discretion.
THERE IS NO AIRPORT PICK-UP AND RETURN OFFERED. Nearest airport is Amarillo, TX (AMA) and is serviced by most major airlines. Auto rental is available there – you will not need your vehicle except to arrive and return from the airport which is about 55 miles from the hunting lodge.
All American Outfitter, Hunt the Texas Panhandle All American Outfitter, Hunt the Texas Panhandle is with Brian Dutrieux.
New #turkeyhunting guests dined on one our favorites - gingered grilled #whitetail backstrap with ginger Demi-glace, ginger rose, wasabi mashed potatoes and baby broccoli with smoked paprika crumbs - to add a little crunch. I love preparing this dish!


text:
CRAZY AMERICA SAYS
local news on a national canvas
Man charged in Illinois bowling alley shooting that killed 3
Florida-based special-forces sergeant allegedly gunned down 6 people, leaving 3 dead, in apparently random attack.
Duke Webb
(Winnebago Sheriff's Office/AP)
A U.S. Army special forces sergeant based in Florida has been charged in an apparently random shooting at an Illinois bowling alley that left three people dead and three wounded, authorities said Sunday.
Winnebago County State's Attorney J. Hanley said Duke Webb, 37, has been charged with three counts of murder and three counts of first-degree attempted murder in the shooting at Don Carter Lanes, in Rockford, on Saturday evening. While no bowling is currently allowed due to state-imposed coronavirus restrictions, a bar linked to the business was legally open.
Webb was taken into custody shortly after the shooting at around 7 p.m., Rockford Police Chief Dan O'Shea said at a news conference Sunday morning.
"I am very confident the officers that were on the scene in the building were able to stop further violence," O'Shea said.
He said the three who died were all men, aged 73, 65 and 69, but did not provide names.
Additionally, he said, a 14-year-old boy was shot in the face and airlifted to a hospital in Madison in stable condition, and a 16-year-old girl who was shot in the shoulder was treated at a hospital and released. A 62-year-old man underwent surgery overnight after suffering multiple gunshot wounds and is in critical condition, the chief said.
The suspect has no known ties to the victims, O'Shea said.
"We believe this was a completely random act, and there is no prior meeting or any kind of relationship between the suspect and any of the victims in this case," O'Shea said. He did not provide information on what led up to the shooting.
The U.S. Army said Webb is a Special Forces Assistant Operations and Intelligence Sergeant assigned to 3rd Battalion, 7th Special Forces Group (Airborne), located at Camp Bull Simons, Eglin Air Force Base, Florida. He joined the Army in 2008 and was on leave Saturday.
"We are shocked and saddened to learn about this tragic event and our thoughts and prayers are with the families of those killed and wounded," Col. John W. Sannes, commander of 7th Special Forces Group, said in a statement.
Maj. Gen. John Brennan, commander of 1st Special Forces Command (Airborne), said in a statement Sunday night that Webb's alleged actions were "abhorrent" and not representative of the Special Forces Regiment. He said actions described in reports were "shocking" and "completely out of character" with Webb's 12 years of honorable service.
The bowling alley was closed at the time of the shooting, in accordance with restrictions imposed to prevent the spread of the coronavirus, O'Shea said. But a bar upstairs was open. The chief said the upstairs venue has double doors that open to the outside, ensuring the bar is in compliance with Illinois' COVID-19 mitigation guidance.
Up to 25 people were at Don Carter Lanes when the shooting happened, but most of them escaped or hid, O'Shea said. He declined to say whether the shootings happened in the bar or elsewhere in the building, saying those details would come out in court. The teens who were wounded were picking up food at the carryout section of the bowling alley, he said.
He said the suspect tried to conceal his weapons before his arrest, and that he was apprehended without officers firing a shot.
"Most of the incident was captured on surveillance video from inside the business," O'Shea said, adding that investigators are studying captured images.
O'Shea said investigators are in touch with the Army. He didn't explain why the Florida man was in Illinois. The Army said it will provide full assistance in the police investigation.
The Rockford Register Star reported that 2020 has been the deadliest year on record for homicides in the city of about 170,000 residents about 80 miles (130 kilometers) northwest of Chicago. Thirty-five people have been killed in the city this year, breaking the previous record of 31 in 1996.
"As we come to the end of this most difficult year and we look ahead at this New Year upon us, we know that this type of violence needs to stop," Mayor Tom McNamara said. "… And today, with the eyes of the country upon us, we need to show as Rockfordians how we respond to an incident such as this, as one Rockford, supporting one another."
ARMED FORCES, ILLINOIS, MURDER, SHOOTINGS
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CRAZY AROUND THE WEB
Instead Of Throwing Out Your Christmas Tree, Why Not Eat It?
In what sounds like a terrifying cookbook, How to Eat Your Christmas Tree, artisan baker Julia Georgallis offers recipes such as Christmas Tree pickles, Christmas-cured fish and Blue Spruce ice cream.
Sword Taken 4 Decades Ago Is Returned To Mass. Community
Someone swiped the sword from a statue of a Revolutionary War general in Westfield, Mass. The thief says he was in college when he went drinking with friends, and woke up with the sword.
Connecticut Dad Says His Daughter Had Her Heart And Her Car Stolen
A woman in South Windsor had been dating her boyfriend for a few months — he'd won over her family. Just after Christmas, her dad says the guy swiped her keys, drove off and didn't come back.
How To Make A New Year's Resolution
A new study looks at ways to make New Year's resolutions succeed.
WATCH: Octopuses Punch Fish, Sometimes For No Apparent Reason
Researchers discovered that an octopus might punch a fish when both are hunting. Although some of the thrown punches can be explained, others remain a mystery.
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text:
Escaping peril »
Escaping peril
NoveList Series:
Wings of fire volume 8
Pub. Date:
0 of 1 Broomfield Children's J Fiction J Suthe
1 of 11 Longmont Junior Fiction J FICTION SUTHERLAND, T.T.
[2016] Scholastic Press 288 pages : illustrations, maps ; 22 cm.
+ Audio CD
0 of 1 Boulder Main Childrens Book CD CD Suth
[2016] Unabridged Scholastic Audiobooks 6 audio discs (approximately 423 min.) : CD audio, digital ; 4 3/4 in.
[2017] Unabridged Findaway World, LLC 1 audio media player (7 hrs., 2 min.) : digital ; 3 3/8 x 2 1/8 in. + 1 AAA battery.
Peril is possibly the most dangerous dragon in Pyrrhia, because she has firescales that can kill an opponent with a touch, but now she has a mission--find her former queen, Scarlet, who is threatening the Jade Mountain Academy, and then stop her, and she is not sure if the persistent SeaWing, Turtle, who is accompanying her, will be a help or a hindrance.
Dragons -- Fiction
Dragons -- Juvenile fiction
Good and evil -- Juvenile fiction
Identity (Psychology)
Identity (Psychology) -- Juvenile fiction
Imaginary wars and battles
Imaginary wars and battles -- Juvenile fiction
Juvenile sound recording
Playaway (Preloaded player)
Prophecies (Occultism)
Prophecies (Occultism) -- Juvenile fiction
Prophecies -- Fiction
Prophecies -- Juvenile fiction
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Quests (Expeditions) -- Juvenile fiction
McManus, Shannon,narrator
Scholastic Audiobooks
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Findaway World, LLC
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Wings of Fire Book Eight:
Wings of fire 8
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Escaping Peril [compact disc] / Tui T. Sutherland
Escaping Peril [electronic resource] / Tui T. Sutherland
Escaping peril / by Tui T. Sutherland
Escaping peril [preloaded player] / Tui T. Sutherland
topic_facet


text:
Le Cubisme est une exposition artistique au Centre national d'art et de culture Georges-Pompidou, à Paris, du  au . Portant sur le cubisme, elle a Brigitte Leal, Christian Briend et Ariane Coulondre pour commissaires.

Liste de quelques œuvres exposées

Anonyme, masque fang.
Anonyme, statue nkisi nkonde, yombé.
Pierre Albert-Birot, La Guerre, 1916.
Constantin Brâncuși, La Muse endormie, 1910.
Constantin Brâncuși, Le Baiser, 1923-1925.
Georges Braque, Le Grand Nu, 1907-1908.
Georges Braque, Arbres à L'Estaque, 1908.
Georges Braque, Le Viaduc à L'Estaque, 1908.
Georges Braque, Les Instruments de musique, 1908.
Georges Braque, Maisons et arbre, 1908.
Georges Braque, La Roche-Guyon, 1909.
Georges Braque, La Roche-Guyon : le château, 1909.
Georges Braque, Broc et Violon, 1909-1910.
Georges Braque, Les Usines du Rio-Tinto à L'Estaque, 1910.
Georges Braque, Clarinette et bouteille de rhum sur une cheminée, 1911.
Georges Braque, Femme lisant, 1911.
Georges Braque, Le Guéridon, 1911.
Georges Braque, Nature morte au violon, 1911.
Georges Braque, Violon, 1911.
Georges Braque, Le Portugais, 1911-1912.
Georges Braque, Compotier, bouteille et verre, 1912.
Georges Braque, Guitare, 1912.
Georges Braque, Femme à la guitare, 1913.
Georges Braque, Guéridon, 1913.
Georges Braque, La Guitare : « Statue d'épouvante », 1913.
Georges Braque, L'Homme à la guitare, 1914.
Georges Braque, Violon et pipe (Le Quotidien), 1913-1914.
Georges Braque, La Musicienne, 1917-1918.
Georges Braque, Café-Bar, 1919.
Paul Cézanne, Cinq baigneuses, vers 1885-1887.
Paul Cézanne, La Table de cuisine, vers 1888-1890.
Paul Cézanne, La Femme à la cafetière, 1890-1895.
Paul Cézanne, Portrait d'Ambroise Vollard, 1899.
Marc Chagall, À la Russie, aux ânes et aux autres, 1911.
Marc Chagall, Les Portes du cimetière, 1917.
Robert Delaunay, La Ville n°2, 1910.
Robert Delaunay, La Ville de Paris, 1910-1912.
Robert Delaunay, Portrait de Guillaume Apollinaire, 1911.
Robert Delaunay, Une fenêtre, 1912.
Robert Delaunay, L'Équipe de Cardiff, 1912-1913.
Sonia Delaunay, La Prose du Transsibérien et de la petite Jehanne de France, 1913.
Sonia Delaunay, Le Bal Bullier, 1913.
Sonia Delaunay, Prismes électriques, 1914.
Félix Del Marle, Le Port, 1913.
André Derain, Nu debout, 1907.
André Derain, Nature morte à la table, 1910.
Marcel Duchamp, Les Joueurs d'échecs, 1911.
Marcel Duchamp, Roue de bicyclette, 1913/1964.
Raymond Duchamp-Villon, Le Cheval majeur, 1914/1976.
Raoul Dufy, Arbres à L'Estaque, 1908.
Serge Férat, Nature morte, 1914.
Paul Gauguin, Soyez mystérieuses, 1890.
Paul Gauguin, Oviri, 1894.
Albert Gleizes, Portrait de Jacques Nayral, 1911.
Albert Gleizes, Les Baigneuses, 1912.
Albert Gleizes, Les Joueurs de football, 1912-1913.
Albert Gleizes, Portrait de l'éditeur Eugène Figuière, 1913.
Albert Gleizes, Portrait d'un médecin militaire, 1914.
Albert Gleizes, Le Chant de guerre, 1915.
Juan Gris, Le Livre, 1911.
Juan Gris, La Guitare, 1913.
Juan Gris, Nature morte au livre, 1913.
Juan Gris, Poires et raisins sur une table, 1913.
Juan Gris, Violon et Verre, 1913.
Juan Gris, Le Papier à musique, 1913-1914.
Juan Gris, Le Petit Déjeuner, 1915.
Juan Gris, Verre et Journal, 1916.
Juan Gris, Nature morte à la plaque, 1917.
Juan Gris, Nature morte sur une chaise, 1917.
Auguste Herbin, Les Trois Arbres, 1913.
Roger de La Fresnaye, Alice au grand chapeau, 1912.
Marie Laurencin, Apollinaire et ses amis, 1909.
Henri Laurens, Tête, 1918-1919.
Henri Le Fauconnier, Le Poète Paul Castiaux, 1910.
Henri Le Fauconnier, L'Abondance, 1910-1911.
Fernand Léger, La Couseuse, 1910.
Fernand Léger, La Noce, 1911.
Fernand Léger, La Femme en bleu, 1912.
Fernand Léger, Le Passage à niveau, 1912.
Fernand Léger, Contrastes de formes, 1913.
Fernand Léger, L'Escalier, 1914.
Fernand Léger, Le Réveil-matin, 1914.
Fernand Léger, Les Maisons dans les arbres, 1914.
Kasimir Malevitch, Samovar, 1913.
Kasimir Malevitch, Croix noire, 1915.
Henri Matisse, Porte-fenêtre à Collioure, 1914.
Henri Matisse, Tête blanche et rose, 1914.
Jean Metzinger, Femme au cheval, 1912.
Jean Metzinger, L'Oiseau bleu, 1913.
Jean Metzinger, Soldat au jeu d'échec, vers 1915-1916.
Piet Mondrian, Paysage avec arbres, 1912.
Piet Mondrian, Composition n°IV / Composition 6, 1914.
Francis Picabia, L'Arbre rouge, vers 1912.
Francis Picabia, La Procession, Séville, 1912.
Francis Picabia, Udnie, 1913.
Pablo Picasso, Portrait de Gertrude Stein, 1905-1906.
Pablo Picasso, Autoportrait, 1907.
Pablo Picasso, Buste de femme, 1907.
Pablo Picasso, Mère et enfant, 1907.
Pablo Picasso, Portrait de Max Jacob, 1907.
Pablo Picasso, Buste de femme, 1907.
Pablo Picasso, Trois figures sous un arbre, 1907-1908.
Pablo Picasso, Cruche, bol et compotier, 1908.
Pablo Picasso, Deux femmes nues debout, 1908.
Pablo Picasso, Nu aux bras levés de profil, 1908.
Pablo Picasso, Nu debout de face, 1908.
Pablo Picasso, Paysage aux deux figures, 1908.
Pablo Picasso, Pains et compotier aux fruits sur une table, 1908-1909.
Pablo Picasso, Maisons sur la colline, 1909.
Pablo Picasso, La Bouteille d'anis del Mono (Nature morte à la bouteille de liqueur), 1909.
Pablo Picasso, Portrait de Fernande Olivier, 1909.
Pablo Picasso, Portrait d'Ambroise Vollard, 1909-1910.
Pablo Picasso, Femme assise dans un fauteuil, 1910.
Pablo Picasso, Femme nue, 1910.
Pablo Picasso, La Femme au pot de moutarde, 1910.
Pablo Picasso, Le Guitariste, 1910.
Pablo Picasso, Portrait de Daniel-Henry Kahnweiler, 1910.
Pablo Picasso, Homme à la pipe, 1911.
Pablo Picasso, Homme à la guitare, 1911.
Pablo Picasso, Homme à la mandoline, 1911.
Pablo Picasso, L'Accordéoniste, 1911.
Pablo Picasso, Mandoliniste, 1911.
Pablo Picasso, Nature morte à la bouteille de rhum, 1911.
Pablo Picasso, Homme à la clarinette, 1911-1912.
Pablo Picasso, Nature morte sur un piano, 1911-1912.
Pablo Picasso, Femme à la guitare, 1911-1914.
Pablo Picasso, L'Aficionado, 1912.
Pablo Picasso, Le Poète, 1912.
Pablo Picasso, Nature morte à la chaise cannée, 1912.
Pablo Picasso, Nature morte espagnole Sol y Sombra, 1912.
Pablo Picasso, Violon, verres, pipe et ancre, 1912.
Pablo Picasso, Le Guéridon, 1913-1914.
Pablo Picasso, Homme à la pipe, 1914.
Pablo Picasso, Le Violon, 1914.
Pablo Picasso, Portrait de jeune fille, 1914.
Pablo Picasso, Cartes à jouer, verres, bouteille de rhum, 1914-1915.
Pablo Picasso, Arlequin et femme au collier, 1917.
Henri Rousseau, La Muse inspirant le poète, 1909.
Léopold Survage, Les Usines, 1914.
Léopold Survage, La Baronne d'Oettingen, 1917.
Henry Valensi, Moscou la sainte, 1912.
Jacques Villon, L'Atelier de mécanique, 1914.

Liens externes

Exposition au centre Pompidou
Cubisme
2018 à Paris
2019 à Paris

redpajama_set_name: RedPajamaWikipedia


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text:
\section{INTRODUCTION}

Young supernova remnants are excellent laboratories for investigating
how stars make elements, and the Crab Nebula in particular can provide unique
information about the precursor star, the supernova event, associated heavy element production,
and the environment of a highly energetic pulsar.  It is the bright remnant
of a core-collapse supernova observed in 1054~A.D.  Its age and location,
roughly 180~pc away from the plane of the Galaxy, suggest that the ejecta
are not significantly contaminated by swept-up interstellar material.
Furthermore, measured electron temperatures in the gas  (Woltjer 1958;
Miller 1978; Fesen \& Kirshner 1982; MacAlpine et al. 1989, 1996) along with
the lack of other possible evidence for shocks (Frail et al. 1995) imply that the line-emitting
gas shines primarily because of photoionization by the locally-generated
synchrotron radiation field (see also Davidson \& Fesen 1985).  Therefore it can be analyzed using powerful
numerical photoionization modeling codes.  It is generally believed that the
supernova precursor star initially contained about $9-11$~M$_{\odot}$ (e.g.,
Arnett 1975; Nomoto 1985), representing the important low end of the Type~II
supernova mass range, below which stars could ignite carbon degenerately and
above which successive nuclear reaction stages would be expected to take place
through silicon burning.  As discussed by Woosley \& Weaver (1986a), the
applicable stellar models allow for a number of explosive and nucleosynthesis
possibilities.

Spectroscopic and photometric investigations of the Crab Nebula to date have
indicated several apparent ``gas components.''  The majority of the observed
nebular gas is helium (e.g., MacAlpine et al. 1989), consisting of less than
$2$ M$_{\odot}$ (MacAlpine \& Uomoto 1991).  It has been postulated that this
represents ``helium mantle'' material from deep within the original star,
ejected by the explosive event.  This is consistent with some stellar models,
or scenarios involving another star, in which outer layers of the precursor were
lost prior to the core-collapse event.  Most of this helium-mantle gas
appears to be nitrogen-rich, confirming its origin from CNO processing
(MacAlpine et al. 1996).

There also is a major component of gas, primarily in the southern part of the nebula
near the pulsar, which is significantly nitrogen-poor and much of which is sulfur-rich
(MacAlpine et al. 1996).  It was suggested that this gas resulted from localized
oxygen-burning episodes, consistent with stellar models (Woosley \& Weaver 1986b, 1995)
that involve off-center (in a shell) oxygen-burning.  Strolger \& MacAlpine (1996)
provided a preliminary demonstration that this explanation is probably correct.

Still another significant nebular component or ``anomaly'' involves an apparent
helium-rich torus viewed as an east-west band across the pulsar region, which constitutes
approximately 25\% of the visible material (Uomoto \& MacAlpine 1987; MacAlpine et al.
1989; MacAlpine \& Uomoto 1991).
The computed helium mass fraction is about 95\%,
and there is not yet a realistic explanation for this apparent structure.

Other known apparent anomalies in the Crab Nebula include exceptionally strong $[$Ni~II$]$
and $[$C~I$]$ line emission, resulting in large spatial variations for deduced
abundances of nickel (along with iron) and carbon.  Strong $[$Ni~ II$]$~$\lambda$7378 has
been reported by numerous authors (Miller 1978; Fesen \& Kirshner 1982;
Henry et al. 1984; MacAlpine et al. 1989).
The latter work suggested neutron-rich
nickel isotopic abundance enhancements, compared with solar, by factors of 5-50 at
various locations.  Iron was also found to vary widely, together with nickel
but at a much lower level; deduced nickel/iron abundance ratios are roughly 60-75
times the solar value.

Henry et al. (1984) found surprisingly high $[$C~I$]$~$\lambda$$\lambda$9823,9850 emission at several
locations in the Crab Nebula, where it was measured to be as much as 7 times stronger
than predicted by the photoionization models of Henry \& MacAlpine (1982).  To
account for this, it was postulated that the $[$C~I$]$ lines might arise from
collisional excitation involving hydrogen atoms as well as electrons.

As part of an effort to develop a more consistent and accurate overall understanding
of the Crab Nebula, we have measured relative line intensities of He~I~$\lambda$5876,
$[$O~I$]$~$\lambda$6300, H$\alpha$, $[$N~II$]$~$\lambda$6583, $[$Ar~III$]$~$\lambda$7136,
$[$Ni~II$]$~$\lambda$7378, $[$S~III$]$~$\lambda$9069, $[$S~III$]$~$\lambda$9531,
and $[$C~I$]$~$\lambda$9850 for roughly 200
well-distributed positions throughout the emitting gas.  In this paper, we address
all of the above issues (apparent gas components and anomalies) using comparisons among
these line measurements.  A follow-up paper, involving more in-depth photoionization
analyses for deriving improved gas physical conditions and chemical abundances,
is planned.

The spectroscopic observations are described in \S~2. Then \S~3 presents
emission-line correlations and resulting inferences about the nebular gas.
The correlations illustrate a broad range of nuclear processing and confirm
significant enrichment with products of oxygen-burning in some areas.
They also suggest two distinct nickel/argon line relationships.
In addition, the importance of optical depth for enhanced $[$C~I$]$ lines is demonstrated,
along with the {\it lack} of a dominant role for optical depth in the production of strong
He~I emission.  A summary discussion is given in \S~4.

\section{OBSERVATIONS}

Spectroscopy covering the wavelength range from approximately 5500 to 7700~\AA\ was
obtained through a long slit at various orientations across the pulsar
during the nights of 1995 January 21 and 22, at the 2.4-m Hiltner
telescope of the former Michigan-Dartmouth-MIT Observatory,
which is located on Kitt Peak.  The Mark~III spectrograph was
used with a TEK~1024$\times$1024 CCD and a 600~lines~mm$^{-1}$ grism blazed
at 5800~\AA, resulting in roughly 2.3~\AA~pixel$^{-1}$ dispersion.
The slit width was 1\farcs2, projected on the sky, and the effective
projected length was about 4\farcm5.  The slit positions employed for
this project are illustrated in Figure~1.  Each involves alignment
through the pulsar and another star, and they are the same as some
of the slit orientations used by MacAlpine et al. (1996), in which extensive
N-rich and N-poor gas components were first identified.
However, the spectral coverage extends further to the red for the
optical observations presented here.

Near-infrared spectral coverage (from 7270 to 10030~\AA) was
obtained during the nights of 2006 January 4 and 5, at the 2.7-m
Harlan J. Smith telescope of the McDonald Observatory.  The Large
Cassegrain Spectrograph was used with the CC1~1024$\times$1024 CCD,
grating No. 42, and an RG610 blocking filter.  The dispersion
through a 2\arcsec-wide slit was about 2.7~\AA~pixel$^{-1}$.
The approximately 2\farcm6-long slit was placed in the positions shown
with darker outlines in Figure~1 (with overlapping coverage
to increase the length in the roughly north-south direction).

Observing conditions on all nights listed above were clear,
and exposure times were at least 1~hour at every slit position.
All of the optical and near-infrared two-dimensional images were carefully
aligned along pixel columns or rows, and the data were reduced
to relative flux against linear wavelength using IRAF\footnote{The Image Reduction and Analysis
Facility (IRAF) is distributed by the Association of Universities for
Research in Astronomy, Inc., under contract to the National Science Foundation.} software,
along with observations of both lamp and moonlit-sky continua, wavelength calibration lamps, and
spectrophotometric standard stars.  Sky spectral observations near the
nebula were employed for removing night sky emission from the
nebular spectra.

The goal was to identify and extract useful one-dimensional
spectra at many positions spatially along the slits.  Resulting
measured line intensities were corrected for differential dust extinction of E(B-V)~=~0.47
(see Davidson \& Fesen 1985 and references therein) using the average
interstellar extinction table from Osterbrock (1989).

To obtain one-dimensional optical spectra, the dispersed radiation
for every spatial pixel along the slits was carefully examined
and compared with the associated two-dimensional image.
Emission knots were identified, and appropriate combinations
of two or three spatial pixels were averaged and extracted for
our measurements.  In all cases, the individual spectral fluxes
for averaged spatial pixels were required to be comparable
(within 25\% of each other), and no single spatial pixels were
used (in order to minimize the possibility of compromising the
data by imperfect dispersion pixel alignment).  Whereas
preliminary measurements were made by more than one person,
all of the data employed here were ultimately, consistently
measured by the first author.

A sample optical spectrum is presented in Figure~2.  This location was
selected for illustration because it has relatively strong
$[$O~I$]$, $[$Ar~III$]$, and $[$Ni~II$]$ lines.  Two emission
systems (e.g., from filaments at the front and back of the
expanding nebula) are often represented in the spectra;
and here a lower-intensity, near-side system with very weak $[$N~II$]$ emission
can also be seen. Sometimes there is
line blending, particularly in the wavelength range with
$[$N~II$]$~$\lambda$6548, H$\alpha$, and $[$N~II$]$~$\lambda$6583.
For such cases,
IRAF deblending routines were employed, and occasionally
the knowledge that $[$N~II$]$~$\lambda$6583~$\approx$~3~$[$N~II$]$~$\lambda$6548 was used
in estimating line fluxes.  In general, repeated
measurements of line fluxes were within 5\% of each other.
Continuum placement in the optical spectra was reasonably
straightforward, and the principal source of error was line
blending.  Experiments showed that using
various reasonable combinations of two or three spatial pixels
at a filament location could lead to measurement
differences up to 25\%, but these changes were always
aligned along, or consistent with, the trends to be
illustrated and discussed in \S~3; so specific pixel selection (following established guidelines)
should not alter the conclusions.  Actual measurement errors for $\lambda$~$<$~7500~\AA\ lines
are estimated to be less than $\pm$10\%.

A sample near-infrared spectrum, illustrating strong $[$Ni~II$]$, $[$S~III$]$,
and $[$C~I$]$ emission, is presented in Figure~3. Whereas there
could have been more than one dynamically different emission system
represented, line blending was never as much of a problem
as in the H$\alpha$ and $[$N~II$]$ region.  Also, we note that these
spectra generally involved larger numbers of averaged pixels
than was the case for the optical spectra. Although the sky
was clear, there were atmospheric seeing problems when the
near-infrared data were obtained.  This and the larger slit
width resulted in somewhat less resolution.
In order to obtain broad wavelength coverage,
potentially useful line-emission positions in each
two-dimensional, near-infrared spectral image were
identified and subsequently located as accurately as possible in the
corresponding optical two-dimensional image.  Then
optimal numbers of pixels were averaged to obtain
consistent (for all wavelengths) one-dimensional spectra for these filaments.
Because of the different slit widths and the fact that
we could not expect exact correspondence between optical
and near-infrared pixel groupings, it was necessary to
normalize the spectra using the overlapped $[$Ni~II$]$~$\lambda$7378
line in both wavelength ranges.  Although these normalization
corrections could be quite accurate and were always less
than a factor of 2, they still provided a significant
potential source of error (estimated as much as 25\%)
when comparing near-infrared and optical line intensities.

Another source of error, for one near-infrared
line, is telluric water vapor absorption.  A plot of measured
and reddening corrected values for $[$S~III$]$~$\lambda$9069 against
$[$S~III$]$~$\lambda$9531 shows a tightly defined linear relation
(with a linear correlation coefficient greater than 0.99),
as it should for emission from two transitions that arise
from the same upper atomic level.   However, the predicted
slope is about 2.6 for $[$S~III$]$~$\lambda$9531 on the vertical axis, according
to the relevant transition probabilities given in the current
NIST Atomic Spectra Database, whereas the slope of the line
in our data is close to 2.0.   This type of situation has
been reported before (Vermeij et al. 2002) and is caused
by water vapor absorption in the 9531~\AA\ wavelength region.
The absorption is clearly seen in our standard star spectra,
and it should not significantly affect either the $[$S~III$]$~$\lambda$9069
or $[$C~I$]$~$\lambda$9850 line measurements.  Because of this, in \S~3
the well-measured $[$S~III$]$~$\lambda$9069 line will be used for examining
spectral trends, rather than the stronger $[$S~III$]$~$\lambda$9531.

\section{TRENDS IN THE DATA}

All measured He~I~$\lambda$5876, $[$O~I$]$~$\lambda$6300, $[$N~II$]$~$\lambda$6583,
$[$S~II$]$~$\lambda$6731, $[$Ar~III$]$~$\lambda$7136, $[$Ni~II$]$~$\lambda$7378,
$[$S~III$]$~$\lambda$9069,
and $[$C~I$]$~$\lambda$9850 emission line intensities were reddening
corrected and normalized to the H$\alpha$ line.
Then they were plotted against each other in various
combinations, as we looked for trends that might provide
new insights for understanding the physical conditions and
chemical abundances in the Crab Nebula, with the future plan
of developing improved photoionization models for the
emitting gas.

\subsection{The Range of Nuclear Processing
and Confirmation of Regions with Enhanced Products
of Oxygen Burning}

As mentioned in the Introduction, MacAlpine et al. (1996)
identified regions in the Crab Nebula with either very
strong or very weak $[$N~II$]$ emission (see their Figure~1).
These gas regimes appear to be distinct both spatially
and dynamically.  The $[$N~II$]$-weak
gas often (but not always, as discussed below) shows
unusually strong $[$S~II$]$ emission, and it was suggested
that the latter probably indicates areas which contain
products of oxygen-burning.  This
would be consistent with some stellar models of Woosley \& Weaver (1986b, 1995).
MacAlpine et al. then used photoionization model analyses
to derive overabundances of nitrogen by factors of 3 to 7
(compared with solar) in $[$N~II$]$-strong regions and
overabundances of Si, S, and Ar (assuming solar nitrogen)
by factors of 10 to 20 for some $[$N~II$]$-weak areas.

Enhanced $[$S~II$]$ emission could also result from
low-ionization, warm H$^{+}$$\rightarrow$H$^{o}$
transition zones in the emitting gas (Henry \& MacAlpine 1982),
wherein S$^{+}$ ions are effectively collisionally excited
by thermal electrons.  Therefore, the hypothesis for oxygen-burning
products should be further investigated and convincingly
demonstrated before its acceptance.  There are ways for
examining this issue with the current data; and the most
straightforward involve correlations between nitrogen and
sulfur emission, between sulfur emission from different
ions, or between emission from different elements
expected to be produced together by the oxygen-burning process.

Figure~4 shows $[$N~II$]$~$\lambda$6583 plotted against
$[$S~II$]$~$\lambda$6731.  We note the large and comparable range
in intensities on both axes.  The nitrogen emission can
be quite strong with very weak sulfur intensities, representing
gas which has progressed no further than the CNO-cycle.
Similarly, the strongest sulfur emission correlates only with
weak nitrogen, suggestive of advanced processing through
oxygen-burning.  It may also be seen that weak nitrogen
does not always correspond with strong sulfur emission,
implying intermediate regions where some helium-burning has taken
place and nitrogen has been converted into neon
(see Pequignot \& Dennefeld 1983; Nomoto 1985; Henry 1986).
Regarding the latter point, infrared neon lines have
been observed in the Crab Nebula by Temim et al.
(2006).  Figure~9 of Temim et al. shows particularly strong
$[$Ne~II$]$~12.8~\micron\ emission in an area roughly 15\arcsec\ SW of the pulsar.
One of the slits used in this study crosses over an emitting filament
at that location, and averages of our measurements there are
$[$N~II$]$~$\lambda$6583/H$\alpha$~=~0.43 and $[$S~II$]$~$\lambda$6731/H$\alpha$~=~1.5.
As may be deduced from our Figure~4, these are low $[$N~II$]$ and modest $[$S~II$]$ values
that could be expected for a region where helium-burning and nitrogen depletion (to neon) have occurred,
but significant oxygen-burning has not taken place.

The data of Figure~4 illustrate the {\it range} of nuclear processing,
but not necessarily the relative {\it amounts} of material for the various
nucleosynthesis stages.  Because of line blending and other factors,
not all emitting positions could be measured and represented.

Figure~5 is a plot of $[$S~III$]$~$\lambda$9069 versus
$[$S~II$]$~$\lambda$6731, which argues that the latter line
does not arise predominantly in optically-thick
H$^{+}$$\rightarrow$H$^{o}$ transition regions.
Even with potential problems involving
normalization of the near-infrared and optical spectra,
there is a reasonably strong
correlation, with a linear correlation coefficient of
0.75 for 37 points.  Therefore, since these different
ionization stages (only one of which might be produced
in an extended low-ionization zone) increase together,
it would appear that strong sulfur emission observed
in the Crab Nebula is mainly a result of enhanced
sulfur abundance.

In addition to sulfur, other primary products of oxygen-burning
include silicon and argon. Silicon emission is
not strong in the optical and near-infrared regions,
but $[$Ar~III$]$~$\lambda$7136 and $\lambda$7751 (weaker) can be measured
in our data.   Therefore, in Figure~6 we plotted
the correlation between $[$Ar~III$]$~$\lambda$7136 and $[$S~II$]$~$\lambda$6731
for 182 locations from the optical
slit spectra.  In this case, there is no potential
problem with spectral normalization, and the correlation
is quite high (linear correlation coefficient of 0.91).
This confirms that the argon and sulfur emission must represent
abundances with a related origin.

Evidence presented here supports the hypothesis
(MacAlpine et al. 1996; Strolger \& MacAlpine 1996)
that certain regions in the Crab Nebula are heavily
enriched with products of oxygen-burning.  This has
important implications for understanding stellar models,
and it will be explicitly considered in our follow-up
photoionization model analyses.  For instance, as
pointed out by Henry (1993), high silicon and sulfur
abundances would cause infrared fine-structure lines
such as $[$Si~II$]$~34.8~\micron\ and $[$S~III$]$~33.6~\micron\
to become more important coolants for the gas, thereby
influencing the line spectra in the optical and near-infrared.
For lower electron temperature, longer-wavelength collisionally-excited
lines such as $[$S~II$]$~$\lambda\lambda$6716,6731 and $[$N~II$]$~$\lambda\lambda$6548,6583
would be enhanced at the expense of shorter wavelength lines like $[$O~II$]$~$\lambda\lambda$3726,3729.
Finally, we note that the above infrared fine-structure $[$Si~II$]$ and $[$S~III$]$
lines were recently observed to have significant
intensities at some locations in the Crab Nebula (Temim et al. 2006).

Products of oxygen-burning are not unique to the Crab Nebula. Cassiopeia A, another young,
collapse-driven, somewhat more massive supernova remnant
also exhibits extensive regions with high concentrations of silicon-group elements like sulfur and argon,
in which it is recognized that oxygen-burning has taken place while silicon-burning has been incomplete
(Chevalier \& Kirshner 1979; Willingale et al. 2002).

\subsection{$[$Ni~II$]$~$\lambda$7378 and $[$Ar~III$]$~$\lambda$7136 Line Trends:
Possible Implications for the Origin of Nickel}

In order to investigate observed very strong nickel
emission in the Crab Nebula,
we plotted $[$Ni~II$]$ intensity against every
other measured line, and we found a particularly interesting correlation
with argon.
In Figure~7, all optical data are presented
for the $[$Ni~II$]$~$\lambda$7378 and $[$Ar~III$]$~$\lambda$7136 lines.
Points below the diagonal show a
linear trend (correlation coefficient of 0.86) involving more highly processed gas,
whereas points above the diagonal show the strongest $[$Ni~II$]$ emission and
tend to represent regions where less nucleosynthesis has occurred.

To investigate or highlight these apparent correlations further, we considered only
data for the very lowest and highest nitrogen emission.
Following guidelines similar to those used by MacAlpine et al. (1996),
we identified the subset of points with measured
$[$N~II$]$~$\lambda$6583~$<$~0.55~H$\alpha$
and $[$N~II$]$~$\lambda$6583~$<$~$[$S~II$]$~$\lambda$6731
as being extreme ``low-N'' locations where
advanced nuclear processing
has taken place.  Similarly those points with
$[$N~II$]$~$\lambda$6583~$>$~3~H$\alpha$ and
$[$N~II$]$~$\lambda$6583~$>$~$[$S~II$]$~$\lambda$6731 were
selected as being ``high-N,'' where nucleosynthesis stopped
with the CNO-cycle.  Figure~8 illustrates
how these data appear in the $[$Ni~II$]$~$\lambda$7378 versus
$[$Ar~III$]$~$\lambda$7136 plane, where filled squares represent
high-N and open squares (with a +) denote low-N.
The separation of trends in
this plot is remarkable, with the low-N (more highly processed) positions
having a linear correlation coefficient of 0.94.

Some points below the diagonal of Figure~7 do not appear in Figure~8,
either because they do not have measurable $[$N~II$]$ emission or because
it is somewhat higher than the imposed limit for inclusion in Figure~8.
We also note that, whereas emission from
several pixel groups along one extended filament might
conceivably create an almost linear structure of
points in a diagram, the measurements
for Figures~7 and 8 come from widely separated
locations in all of the slits.

The linear correlation between $[$Ni~II$]$ and
$[$Ar~III$]$ emission from the most highly processed gas
could result from a type of ``alpha-rich freezeout''
(see Woosley \& Weaver 1995; Jordan et al. 2003), whereby
silicon-group elements in core-collapse supernovae may be heated by a shock wave
and broken down into nucleons and alpha particles.
Then, as the gas cools, these particles can reassemble into various stable iron-peak nuclei.
Another possibly contributing process has been discussed
by Thielemann \& Arnett (1985), who wrote:
``During O-burning, temperatures favor the photodisintegration
of heavy nuclei (produced by the s-process) into Fe-peak nuclei.
This is seen for $^{60}$Ni and partially for $^{62}$Ni and $^{58}$Fe,
depending on the prior neutron excess $\eta$.''

The above explanations would not
apply to the steeper correlations in Figures~7 and 8, where
$[$Ni~II$]$~$\lambda$7378 can be strongest in less-processed gas.
This may be an indication that some
iron-peak, neutron-rich nuclei were removed from the
surface of the neutron star.  For
pulsars in general, this possibility was
investigated by Ruderman \& Sutherland (1975),
who concluded that extremely strong surface magnetic
fields would not permit
the release of heavy ions for most pulsars.  However, they
also stated that the Crab Nebula's neutron star may be an
exception to this rule because of very high surface temperature.
In this regard, we note that an extremely high temperature region on this
young neutron star may have been detected by Weisskopf et al. (2004).
Furthermore, Michel et al. (1991) mapped an extensive north-south
relativistic wind for the nebula,
in the directions of the highest apparent
concentrations of nickel (MacAlpine et al 1989).
For line-emitting knots immersed in this wind, the highest $[$Ni~II$]$ emission was
measured on the side facing the pulsar in each
case (MacAlpine et al. 1994; MacAlpine \& Lawrence 1994).
As Freiburghaus et al. (1999) have noted, the origins
of neutron-rich heavy elements are not yet well understood.
If ions can leave the surface of the neutron star in the
Crab Nebula, then young pulsars in general could represent
sources for some heavy nuclei.

\subsection{On The Origin of Strong $[$C~I$]$ Emission}

Henry et al. (1984) measured the strength of $[$C~I$]$~$\lambda$9850
in some filaments to be at least several times stronger
than predicted by their photoionization models, and
they suggested that previously neglected collisional
excitation by H$^{0}$ may need to be considered as a
potentially important process for production of this
emission.

If we can understand where and how the $[$C~I$]$ emission
is produced, we may be able to use it for estimating
the carbon abundance relative to other elements.
This, in turn, could provide additional useful insights
into the extent of nuclear processing at various locations.
As noted by Nomoto (1985) and Henry (1986), the amounts
of carbon and oxygen would be depressed somewhat by
CNO~processing and then would increase (above solar)
as a result of helium-burning.  Also, Nomoto pointed
out that an improved understanding of the carbon
abundance, and therefore the amount of processing in
the gas, can lead to a more accurate estimate of the
stellar precursor mass.  Whereas carbon abundances
derived from ultraviolet lines like C~IV~$\lambda$1549 for the
Crab Nebula may be significantly influenced by the
way in which absorption of He~II~$\lambda$304 photons is
considered (Eastman et al. 1985), that complication should not be
an issue for the $[$C~I$]$~$\lambda$9850 line, since
it arises away from the He~II-emitting gas.

New insight regarding the production of $[$C~I$]$ emission
may be gained from examining its correlation with $[$O~I$]$.
As previously shown in Figure~2, the Crab Nebula contains
some locations with particularly strong $[$O~I$]$~$\lambda$6300
emission, probably indicating the existence of broad
H$^{+}$$\rightarrow$H$^{o}$ transition zones in the gas.
The $[$O~I$]$ emission is known to be strengthened in these warm
low-ionization regions (which could be expected for
photoionization by a relatively flat synchrotron spectrum)
because O$^{0}$ follows H$^{0}$ due to very effective charge
exchange interactions.

Figure~9 illustrates the correlation between our measured
$[$C~I$]$~$\lambda$9850 and $[$O~I$]$~$\lambda$6300 intensities.
Although the plot is affected by the spectrum normalization
procedure for near-infrared and optical wavelengths, the
linear correlation coefficient is a significantly high 0.81.
Therefore, we conclude that the strong $[$C~I$]$ emission is probably enhanced
in extended ionization transition zones, by electron collisional excitation
and perhaps also by collisions involving H$^{0}$.  However, since
the C and O contents of the gas could also have been depleted
or increased {\it together} by the CNO-cycle or helium-burning,
additional information is needed.

{\it Indirect} support for the idea that $[$C~I$]$ emission must be strengthened in
low-ionization regions also comes from Figure~10, which shows $[$C~I$]$~$\lambda$9850
plotted against $[$N~II$]$~$\lambda$6583.  There is a rather large
(though not extreme) range of $[$N~II$]$ emission represented,
and (except for the one very high point) $[$C~I$]$ looks
random over an order of magnitude in the $[$N~II$]$ intensities.
Since the latter may provide a rough representation of the
amount of nucleosynthesis that has taken place, as
discussed previously, it would appear that the strong measured
$[$C~I$]$ emission is not directly correlated with nuclear processing.
Clearly the roles of both abundance and ionization structure will be important
avenues for exploration in further refinements of
photoionization model computations.

\subsection{Exceptionally Strong He~I Emission}

The final abundance or line-intensity anomaly to be
considered here involves the exceptionally high helium content
derived by MacAlpine et al. (1989) for an apparent
helium torus around the pulsar (see also Lawrence et al. 1995).
Having measured dereddened He~I~$\lambda$5876~$\gtrsim$~H$\beta$,
the results of photoionization analyses by Henry and MacAlpine (1982)
were used to infer a helium mass fraction around 95\% in this region.

Henry \& MacAlpine (1982) also considered the possibility that
He~I~$\lambda$5876 recombination lines could be significantly enhanced
relative to hydrogen emission in low-ionization zones.
Because the photoionization cross
section for He$^{0}$ scales roughly with frequency as $\nu$$^{-2}$,
whereas that for H$^{0}$ scales more like $\nu$$^{-3}$, a high
energy synchrotron radiation field can continue to ionize helium
significantly beyond where hydrogen starts
becoming neutral, thereby producing excess He~I recombination emission.
This process could be especially
important if the ionizing radiation flux is low (see, e.g., Shields 1974).
However, Henry \& MacAlpine found that photoionization
models with relatively high values for the ionizing
flux did a much better job of matching the majority of observed
line intensities in the Crab Nebula, so they favored
very high derived abundance as the most plausible
explanation for the strongest helium
intensities. Now we have the opportunity to investigate this further.

As with $[$C~I$]$ emission, we examined
the relation between He~I~$\lambda$5876 and $[$O~I$]$~$\lambda$6300 for
our data, as shown in Figure~11.
It may be seen that evidence for a meaningful correlation is lacking.
Strong He~I emission is similarly represented at both
high and low $[$O~I$]$ intensities, so it is not
enhanced primarily in low-ionization gas.  Furthermore,
we considered the He~I~$\lambda$5876 correlation with $[$N~II$]$~$\lambda$6583
in Figure~12.  Again, the strongest He~I emission is evident with both
high and low $[$N~II$]$ measurements, so it apparently is not
directly tied to the overall progress of nuclear processing.
We conclude that the most reasonable explanation for
the strongest He~I lines in the apparent torus around the pulsar
is anomalously high abundance, the source of which is still
in need of a plausible explanation.

\section{SUMMARY}

We have measured emission of He~I~$\lambda$5876, $[$O~I$]$~$\lambda$6300,
$[$N~II$]$~$\lambda$6583, $[$S~II$]$~$\lambda$6731,
$[$Ar~III$]$~$\lambda$7136, $[$Ni~II$]$~$\lambda$7378,
$[$S~III$]$~$\lambda$9069, $[$S~III$]$~$\lambda$9531,
and $[$C~I$]$~$\lambda$9850 at many locations
within the Crab Nebula.  The different line intensities
(or subsets thereof) were plotted against each other
in efforts to investigate correlations and improve our understanding of the range
of nuclear processing in the gas, as well as the causes
of exceptionally strong emission from $[$Ni~II$]$, $[$C~I$]$,
and He~I.  We identified gas where nucleosynthesis
has not progressed significantly beyond the
CNO-cycle, gas in which some helium-burning and nitrogen depletion have taken
place, and regions where oxygen-burning has occurred.
The anomalously strong observed $[$Ni~II$]$ emission may have
two sources, in one case resulting from high temperature
and subsequent cooling in gas enriched with products of oxygen-burning,
while in the other case possibly representing the release
of nuclei from the neutron star surface.  Line correlations
indicate that very strong $[$C~I$]$ emission
arises in low-ionization H$^{+}$$\rightarrow$H$^{o}$ transition regions.
On the other hand, exceptionally strong He~I~$\lambda$5876
does not show similar evidence of a low-ionization zone origin; and it does not appear to
correlate with different levels of nuclear processing
as represented by $[$N~II$]$ emission.  Therefore, the apparent
high-helium torus around the pulsar may be a distinct component
of the nebula.

\acknowledgments

We are grateful for generous financial and logistical support
from Trinity University and the endowed Charles A. Zilker Chair position.
We also thank the staffs of the Michigan-Dartmouth-MIT Observatory
and the McDonald Observatory for providing excellent technical
assistance with this research.

redpajama_set_name: RedPajamaArXiv


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Using a combination of CIAO tools, we extract source and background spectra for an extended source. The background spectrum is grouped, if desired. The appropriate Response Matrix Files (RMFs) and Ancillary Response Files (ARFs) are created for both source and background.
The specextract script automates these steps for extended and pointlike sources observed with the ACIS detector.
To generate source and background spectra of an extended ACIS source and build the proper RMFs and ARFs.
The Extract Spectrum and Response Files for a Pointlike Source thread handles the pointlike source case.
Last Update: 17 Dec 2014 - Reviewed for CIAO 4.7; removed "New in CIAO4.6" sections. Minor edits.
dsAPEPULSEHEIGHTERR -- WARNING: pulse height is less than split threshold when performing serial CTI adjustment.
As only a small number of events are reported, the warning can be ignored.
dmextract: to extract source and (optionally) background spectra. This tool also creates the WMAP used as input to mkacisrmf.
sky2tdet: to create the WMAP input for mkwarf.
mkwarf: to create weighted ARF(s).
mkrmf or mkacisrmf: to build the RMF(s), depending on which is appropriate for the data and the calibration; see the Creating ACIS RMFs why topic for details.
dmgroup: to group the source spectrum and/or background spectrum.
dmhedit: to update the BACKFILE, RESPFILE and ANCRFILE keys in the source and background spectrum files.
Weighted ARFs are generated by default, since weight=yes. For point-source analysis, or when you are not interested in the spatial variation of the effective area, unweighted ARFs can be calculated by setting weight=no.
RMFs are - by default - generated without any weighting, since this can considerably speed up the running of the script and - for most cases - does not significantly change the result, since the RMF variation with position is small. If you do want to create weighted RMF files, then set weight_rmf=yes and weight=yes.
Users can also specify a location at which to calculate unweighted responses - using the refcoord parameter - rather than using the location of the source and background regions.
The regions are shown displayed on the event file in Figure 1.
The background was chosen from a source-free area of the same chip for this example, but it may also be chosen from a different chip or different event file.
Choose the background from another same-type chip that was on in the observation. If your source is on ACIS-S3 and ACIS-S1 (the other back-illuminated chip) was also turned on, define the background on ACIS-S1.
If using another chip from the observation is not an option, use one of the ACIS "blank-Sky" background files which are distributed in the CALDB.
If you plan on using one of the ACIS "blank-sky" background files from the CALDB and intend to subtract the background spectrum (i.e. not fit it), then you do not need to create a background RMF and ARF. Set the bkgresp parameter to "no" and the script will only extract a background spectrum.
Omit the background completely (i.e. leave the bkgfile blank).
Updating header of simple.pi with RESPFILE and ANCRFILE keywords.
Updating header of simple_grp.pi with RESPFILE and ANCRFILE keywords.
Updating header of simple_bkg.pi with RESPFILE and ANCRFILE keywords.
Updating header of simple.pi with BACKFILE keyword.
Updating header of simple_grp.pi with BACKFILE keyword.
The contents of the parameter file may be checked with plist specextract.
If you want more details on what the script is doing, set verbose=2 before running specextract.
The above call created an ARF and RMF for the background region; if you only intend to subtract the background, rather than fitting it, you do not need these responses so can save time (particularly if the background area is large) by setting bkgresp=no when running specextract.
We choose to use the default grouping values: the source spectrum will be grouped to a minimum number of 15 counts per new channel and the background spectrum will be ungrouped. The grouptype and binspec parameters are used to specify the source spectrum grouping, and the bkg_grouptype and bkg_binspec parameters specify the background spectrum grouping.
The energy_wmap parameter determines the energy band used to create the weight map when weight=yes.
If you use the soft band (e.g. the default value of 300:2000 eV), then you are weighting by the emission from the source (unless you have a very hard spectrum). To weight by the effective area of the telescope (again, unless you have a hard source), set the range to, for example, 2000:7000 eV.
Unless the spectrum of your source is unusual, adjusting the WMAP energy range will not affect the ARF - or,	therefore, the spectral fit - noticeably.
This section explains how to manually run the analysis steps that are used by specextract.
Make sure that you have set up ardlib to use the bad pixel file for your observation before following this section of the thread.
First, we extract spectra from the events enclosed by the source and background regions.
To create a WMAP block in a PHA file, dmextract must be given a binning specification for its wmap option. This WMAP will be used as input to mkacisrmf. It must be in detector coordinates, and the suggested binning factor is 8; an optional energy filter is included for the WMAP.
unix% pset dmextract infile="acisf00869_repro_evt2.fits[sky=region(simple.reg)][bin pi]"
unix% pset dmextract wmap="[energy=300:2000][bin tdet=8]"
unix% pset dmextract infile="acisf00869_repro_evt2.fits[sky=region(simple_bkg.reg)][bin pi]"
You can check the parameter file that was used with plist dmextract.
We now need to create the aspect histogram, which is a binned representation of aspect motion during the observation.
The contents of the parameter file may be checked with plist asphist.
The WMAP created by sky2tdet properly weights the ARF based on how much of the source flux fell onto the bad pixels, columns, or a node boundary, and which bad pixels are actually exposed. Without accounting for these effects, the ARF is over-estimated.
unix% pset sky2tdet infile="acisf00869_repro_evt2.fits[sky=region(simple.reg)][energy=300:2000][bin sky=1]"
If you made a separate aspect histogram for the background, set it in the asphistfile parameter before running the tool for the background spectrum.
unix% pset sky2tdet infile="acisf00869_repro_evt2.fits[sky=region(simple_bkg.reg)][energy=300:2000][bin sky=1]"
You can check the parameter file that was used with plist sky2tdet.
mkwarf creates a weighted ARF file based on the WMAP that was created with sky2tdet. It also produces a set of weights that are used by mkrmf to create the associated weighted RMF.
You can check the parameter file that was used with plist mkwarf.
The observation used in this thread (ObsID 869) was taken at the -120 C focal plane temperature. Therefore, mkacisrmf should be used to create the RMF file.
The syntax for both mkacisrmf and mkrmf are given in this section. Users should choose the appropriate tool for the data and calibration.
The mkacisrmf why topic has more details on using the mkacisrmf tool.
The RMF doesn't change quickly enough to require the detail of the sky2tdet WMAP, and its precision will cause mkacisrmf to run very slowly. Nearly identical results are obtained with the dmextract WMAP with a more reasonable runtime.
You can check the parameter file that was used with plist mkacisrmf.
You can now skip to the Update the Spectrum Files section.
The mkrmf tool uses the weightfile from mkwarf to create the weighted RMF. The tool queries the CALDB for the correct FEF file and the energy axis grid is ignored since the grid is read from the weights file. Note that although the axis1 parameter is ignored, a syntactically-correct value must be entered; this example uses axis1="energy=0:1".
You can check the parameter file that was used with plist mkrmf.
Sherpa has dynamic grouping capabilities so you can easily set or change the grouping of a dataset at the Sherpa prompt. For other data analysis packages it can be useful to create a grouped version of the spectrum as a seprate file.
You can check the parameter file that was used with plist dmgroup.
Finally, update the appropriate header keywords in the both the ungrouped and grouped source files.
Note that the ungrouped background file name is used as the BACKFILE header keyword value. The source grouping is applied to the background grouping when fitting in Sherpa. For fitting only background data, or simultaneous fitting of source and background data, Sherpa can group background dynamically with the group functions; see the Fitting section of this thread for more information.
In this example, we show how specextract can create multiple output spectra from a single run of the script.
This example uses two observations of G21.5-09. Both observations will be processed by specextract at the same time, producing two sets of output files; this is explained further in the Run specextract section.
and then use reproject_obs to reproject the data sets to a common tangent-plane position (i.e. so that the SKY coordinate system is the same in the two event files).
New tangent point: RA=18h 32m 21.696s Dec=-10d 34' 41.484"
Reprojecting 2 event files to a common tangent point.
As the screen output describes, the merged event file - in this case reproj/merged_eve.fits - should not be used for spectral analysis.
The regions are shown displayed on the event files in Figure 2.
ObsID 1842 is displayed in the top frame and ObsID 1843 is displayed in the bottom frame.
Using an external file for a stack - such as multi_src.lis and multi_bg.lis - is useful when either the contents are going to be used multiple times or the contents are long, but you can also use a comma-separated list of values, which is what we do for the stack of output names (the outroot parameter). If you prefer, you may just give a single value for outroot and specextract will create output files designated as "src1", "src2", "bkg1", "bkg2", etc. The default values for combine, weight, and correctpsf (no, yes, and no respectively) are used. In the output below the bold lines show the ancillary files that were selected by the script.
WARNING: A supported spatial region filter was not detected for @multi_src.lis, which is required input for point-source analysis with ARF correction.
WARNING: A supported spatial region filter was not detected for @multi_bg.lis, which is required input for point-source analysis with ARF correction.
Updating header of spec/1842.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1842_grp.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1843.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1843_grp.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1842_bkg.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1842.pi with BACKFILE keyword.
Updating header of spec/1842_grp.pi with BACKFILE keyword.
Updating header of spec/1843_bkg.pi with RESPFILE and ANCRFILE keywords.
Updating header of spec/1843.pi with BACKFILE keyword.
Updating header of spec/1843_grp.pi with BACKFILE keyword.
These responses are weighted and there are responses for the background spectra, since weight=yes and bkgresp=yes.
The red curve shows the data after background subtraction whereas the black curve includes the background contribution.
If you would like to fit the background-subtracted source spectrum using a common RMF and ARF for source and background, simply read the source spectrum FITS file into Sherpa, subtract the background, and fit. See the Introduction to Fitting PHA Spectra thread for details.
To fit source and background spectra simultaneously with distinct RMFs and ARFs, follow the Independent Background Responses thread.
The RESPFILE and ANCRFILE header keywords in the source and background spectra have been updated, as well as the BACKFILE in the source spectra. This means that when the spectra are read into Sherpa, all the supporting files will automatically be read as well; the background (if available) will be defined, as will the source and background response files.
Users should be cautious about analyzing the data for sources near the edges of the ACIS CCDs.
For X-rays passing through the mirrors, the very bottom of each CCD is obscured by the frame store. As a result, some of the events in rows with CHIPY <= 8 are not detected. (The set of rows affected varies from CCD to CCD.) Since the CIAO tools do not compensate for this effect, the ARFs and exposure maps for sources in these regions may be inaccurate.
For sources within about thirty-two pixels of any edge of a CCD, the source may be dithered off the CCD during part of an observation. The aspect histogram, which is used to create ARFs and exposure maps, is designed to compensate for this effect.
An ARF calculated at the edge of a chip will not be accurate since the response tools for spectral extraction (specifically the ARF) assume that 100% of the PSF is enclosed - i.e. on the chip - all the time, which may not be the case. The amount of error introduced depends on how close the source is to the edge, the morphology of the source, and the characteristics of the PSF, which depends on the source spectrum.
A contaminant has accumulated on the optical-blocking filters of the ACIS detectors, as described in the ACIS QE Contamination why topic. Since there is a gradient in the temperature across the filters (the edges are colder), there is a gradient in the amount of material on the filters. (The contaminant is thicker at the edges.) Within about 100 pixels of the outer edges of the ACIS-I and ACIS-S arrays, the gradient is relatively steep. Therefore, the effective low-energy (' 1 keV) detection efficiency may vary within the dither pattern in this region. The ARF and instrument map tools are designed to read a calibration file which describes this spatial dependence.
(bkgresp = yes)             Create background ARF and RMF?
(weight = yes)             Should response files be weighted?
(weight_rmf = no)              Should RMF also be weighted?
(refcoord = )                RA and Dec of responses?
(correctpsf = no)              Apply point source aperture correction to ARF?
(combine = no)              Combine ungrouped output spectra and responses?
(clobber = no)              Remove existing files?
(clobber = no)              overwrite existing output file (yes|no)?
(clobber = no)              Clobber existing output file?
12 Jan 2010 updated for CIAO 4.2: specextract uses a CALDB query to decide which RMF tool should be used; calibration update - the ACIS QE contamination model has been upgraded to vN0005.
09 Mar 2010 The ACIS detector is calibrated over the range 0.224004 - 12 keV; choosing values outside this range will result in errors from specextract.
04 Apr 2011 updated for 04 Apr scripts package release: acis_fef_lookup script prints the version at verbose > 0. specextract: user is prompted for the bkgfile parameter (previously was hidden); new parameter, bkgresp, determines whether a background ARF and RMF should be created; additional changes are outlined in detail in the script release notes for 04 Apr 2011.
12 Apr 2011 updated for 12 Apr scripts package release: specextract bug fix - regions may be specified on the command line or in a file, i.e. "sky=circle(344,435,10)" vs. "sky=region(src.reg)".
16 Feb 2012 a specextract bug fix was released in the 16 Feb 2012 scripts package: the script will not error out if you set outroot to be a stack and have correct=yes and weight=no.
08 Aug 2013 Updated for the contributed scripts 4.5.4 release: the "ancillary" files - e.g. aspect solution and bad-pixel files - can now be picked up from information in the event file (in many cases). The Extracting Multiple Spectra section has also been updated.
12 Dec 2013 Review for CIAO 4.6: by default weighted RMF files are no-longer generated; the pbkfile parameter has been removed from specextract and is no-longer used by tools like mkwarf; the response files are now always named with the .rmf and .arf suffix, even when weighted; the multiple spectra section now uses reproject_obs to align the observations before source extraction; although not shown in this thread, specextract can now be used with HRC-I data sets.
17 Dec 2014 Reviewed for CIAO 4.7; removed "New in CIAO4.6" sections. Minor edits.


text:
Reporter removed from Catawba Nation meeting, cited for trespassing: Sheriff
by: Jesse Ullmann
ROCK HILL, S.C. (QUEEN CITY NEWS) – A reporter who was covering a Catawba Nation meeting this weekend near Rock Hill was removed from the meeting and cited for trespassing, Queen City News has confirmed.
The Post and Courier, which covers news across the state of South Carolina with roots in Charleston, said on Saturday that one of its reporters, Maggie Brown, had been charged with trespassing while covering a Catawba Nation meeting.
Brown is a beat reporter for the Post and Courier in the Rock Hill area, part of the paper's statewide coverage plan, and is a native North Carolinian, according to the newspaper's website. Brown had been working on a story about the Native American Catawba Nation tribe cutting ties with its casino partner amid federal scrutiny.
Kings Mountain casino found in violation of federal law; could face temporary closure
Last month, a notice of violation was issued last month against the Catawba Indian Nation and its Two Kings Casino partners by the National Indian Gaming Commission for expanding the casino without an approved management contract. "We issued a Notice of Violation to both enforce regulatory compliance and ensure the Nation is the primary beneficiary of its gaming revenue," the commission said in a statement released at the time. The partners are Kings Mountain Sky Boat Partners, LLC (Sky Boat), and Sky Boat's owners. The investigation was conducted by the commission's D.C. bureau. Penalties at the time were said to have included a possible daily $57,000-pluss fine.
Push for sports betting in NC heats up
Saturday's meeting had over 200 people in attendance and was held on the reservation near Rock Hill to discuss those ties with its casino partners, the newspaper said. The sheriff's office said the meeting was not open to the public. Brown was removed from the meeting, handcuffed, and placed in the back of a cruiser, before being released, the article said. The York County Sheriff's Office told Queen City News that Brown was given a citation for trespassing and released. Brown had requested to attend the meeting prior to the incident and was denied by the tribal administration, according to the sheriff. A request for a comment from the newspaper's editor was not immediately responded to.
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Catawba Two Kings Casino opened in 2021. "Anytime you go there, late at night, the parking lot is full," Kings Mountain Mayor Scott Neisler told Queen City News shortly after its debut.
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Last year right before the start of the current NFL season, a 24-hour sports book featuring 30 kiosks opened inside the casino.
Catawba Nation said Brown has been banned from tribal lands and released the following statement on Sunday.
There is an unfortunate and long history of non-Native people not respecting the lands, laws, and traditions of Native people. During a General Council meeting of Catawba citizens yesterday, Post and Courier reporter Maggie Brown Driggers chose to add to this history.
Catawba General Council meetings are gatherings of Catawba citizens to discuss, debate, and ultimately vote on issues facing the Nation. These meetings are open only to Catawba citizens and invited guests. We are a sovereign nation with the power to set boundaries and laws on our land to protect and serve our people. This includes restricting those who are allowed and not allowed in our meetings.
Yesterday, a reporter from the Post and Courier attended a meeting without identifying herself and after receiving a message denying her access to the meeting in previous correspondence from the Nation. Maggie Brown Driggers' actions make clear that she was aware that this meeting was not open to uninvited non-Catawbas, and despite this she chose to ignore our boundaries.
Once discovered, she was asked to leave the meeting and arrested for trespassing. Due to the intentional disrespect she demonstrated, the General Council of the Catawba Nation voted to ban Maggie Brown Driggers from Tribal lands.
We have held many General Council meetings over many years and have never had a media organization ignore our laws and violate our sovereignty in such a way. We welcome media organizations who follow our procedures, as well as respect our laws and our community. The Nation hopes to work on improving our relationship with the Post and Courier in the future.
We also note that Maggie Brown Driggers reported on her arrest last night without mentioning the myriad of ways she knew that she was not invited to our General Council meeting and was violating our laws. Accuracy, truth, and accountability are bedrock principles of journalism, and we are disappointed that Mrs. Brown Driggers does not feel those principals apply to her own actions.


Check out this iPhone segment on the Today show this morning. Maybe the iPhone's not that easy to use after all. Or maybe the problem is between phone and seat. We have to laugh at the mainstream media's satellite shot, just like from the '60s, trying to show that the iPhone can make calls everywhere, even from New York to frickin' London! But then, with all that satellite tech brought to bear, the anchorette can't even answer that complicated iPhone. It's called a touchscreen, Meredith!


The film plays with the established rules in ways that are clever, consistent, and yield brilliant results...always a tricky mix for any movie that deals with the paradoxes of time travel, and the director and a game cast of bright young things pull it off in spades.
"Time Lapse" works due to both their escalating pileup of well-thought-out complications and credible character psychologies nicely communicated by expert performances.
Three friends discover a mysterious machine that takes pictures 24hrs into the future. When they start to use it for personal gain, the machine takes over their lives and controls their future, with devastating results.


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