For the enterprise, Java and Microsoft's .NET rule. However, Java has the edge, as it is No. 1 language in terms of number of developers.
C# is a multiparadigm programming language encompassing imperative, functional, generic, object-oriented and component-oriented programming disciplines. Microsoft developed C# within its .NET initiative and the language was later approved as a standard by Ecma and ISO. C# also is slated by Microsoft to become the primary development language for Windows Phone 7. Like Java, C# is big in the enterprise. However there are considerably fewer C# developers than there are Java developers. But the importance of C# as part of the Microsoft .NET strategy and its support through the Visual Studio tools suite make C# a formidable contender in the programming language race. C# ranked No. 6 on the most-recent TIOBE Index.
We know they are not the same language, though C++ builds on C and began as an extension of the C language. Though sometimes viewed as "nichey," C++ is widely used in the software industry. Some of its key application domains include systems software, application software, device drivers, embedded software, high-performance server and client applications, and entertainment software such as video games. C++ has greatly influenced many other popular programming languages, most notably Java. Furthermore, C and C++ ranked No. 2 and 3, respectively, on the most-recent TIOBE Index.
Like the BASIC programming language, Visual Basic was designed to be easily learned and used by beginner programmers. The language not only allows programmers to create simple GUI applications, but it can also be used to develop complex applications. Programming in VB is a combination of visually arranging components or controls on a form specifying attributes and actions of those components, and writing additional lines of code for more functionality. With ease of use as a selling point, Visual Basic caught on like wildfire. There is simply too much VB code out there to ignore this language in any list of 10 programming languages. Visual Basic ranked No. 5 on the most-recent TIOBE Index.
PHP is very popular for corporate applications and for Web design. If you want to be a freelancer it's a good language to know. PHP was designed as a general-purpose scripting language that was originally designed for Web development to produce dynamic Web pages. PHP was ranked No. 4 on the most-recent TIOBE Index.
If you want to make a lot of money, but probably also work on very intense high-pressure projects where risk is often involved—as in a lot can go wrong—learn Objective-C. Objective-C borrows from Smalltalk and the C language, and it influenced the creation of Java. Objective-C is used primarily on Apple's Mac OS X and iOS. With the wild popularity of Apple's iPhone, iPod Touch and iPad, there are simply not enough Objective-C developers out there to meet the needs of users hungry for more apps for these devices. Objective-C ranked No. 9 on the most-recent TIOBE survey, but that is up from being No. 45 in the survey in June of 2009.
Many say Perl is the new COBOL. Perl is also viewed as "the duct tape of the Internet" and is used to integrate databases and other systems together. While demand for the dynamic or scripting languages such as Perl, Python, PHP and Ruby lags behind that of Java and more mainstream languages, the popularity of these languages is growing and there is a need for programmers in each of those communities. However, according to Indeed.com, the demand for Perl programmers is tracking higher than that for PHP, Python and Ruby developers, in that order. Perl was ranked No. 8 on the most-recent TIOBE Index.
Want to work on the leading edge and build applications for the cloud? Dynamic languages, especially Python, are being used to create Web/cloud applications on frameworks such as Django. Google App Engine is built with Python and originally only supported Python. The advantage of Perl and Python over PHP among the dynamic languages is that while PHP is a Web-only, server-side language, Perl and Python are both general purpose languages with usage in multiple industries, from aerospace and defense to sciences and to financial to hi-tech. Python was ranked No. 7 on the most-recent TIOBE Index.


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Heat oven to 375° F. Lightly coat a 9-inch round cake pan with vegetable cooking spray.
Finely chop the almonds. Grate 1 teaspoon orange zest from one of the oranges and cut strips of zest from another to use for garnish. Squeeze 1 1/2 cups juice from the oranges.
Prepare the muffin mix according to the label directions but substitute 3/4 cup of the orange juice for water and blend in the chopped almonds and grated zest. Pour into pan. Bake 25 minutes or until a toothpick inserted in the center comes out clean. Cool torte in pan on a wire rack for 10 minutes. Remove from pan.
Meanwhile, in a small saucepan, combine the sugar and the remaining 3/4 cup orange juice. Simmer, stirring occasionally, until slightly reduced and thickened, about 10 minutes. To serve, spoon the sauce over the torte and garnish with the orange-zest strips.
I've made this several times --- each time getting tons of compliments ! Very easy recipe and makes a wonderful presentation !


This is a very beautiful attraction, located some thirty four kilometers north-east of the city of Puno, in the province and department of the same name. Sited opposite the Archeological Complex of Sillustani, it is surrounded by areas of marshland and pasture, which flood on a seasonal basis. It has a maximum depth of 27 meters and connects to Lake Titicaca via the River Illpa.
In its central part lies the island of Umayo, which has its own flora and fauna as well as introduced species such as vicuñas, guanacos and deer. Its water level fluctuates, and is at its lowest during the months of July and September.
Various activities related to tourist hospitality are available in the immediate vicinity of the lake, which allow visitors to learn more about the local way of life. Some families have adapted their homes to offer accommodation to tourists. They do demonstrations of sowing, weaving with alpaca and sheep wool, and animal husbandry. Hikes with llamas and boat rides on Lake Umayo are also offered, as well as activities such as herding domestic animals and participating in other farming activities.


text:
Big band music Jazz Jazz (Chants) États-Unis Jazz 1941-1950 Jazz 1951-1960 Jazz 1961-1970 Jazz vocals Piano music (Jazz) Saxophone music (Jazz) Trumpet music (Jazz)
Armstrong, Louis Basie, Count Ellington, Duke Evans, Gil Getz, Stan Haynes, Roy. Horne, Lena. McGhee, Howard Tatum, Art Tristano, Lennie.
Charles Mingus, the complete 1959 Columbia recordings Charlie Saunders Collection Charllie Saunders Collection Chess reissue ; 0001 Columbia jazz Great American composers Great jazz composers series Jazz series (Clef)
bibliography Blues (Music) Concert films. Jazz Jazz. Live sound recordings. Long-playing records. Nonfiction films. Phonograph records. Vocal
Louis Armstrong plays W.C. Handy.
Handy, W. C. (William Christopher)
Contents: St. Louis blues (8:50) -- Yellow dog blues (4:16) -- Loveless love (4:28) -- Aunt Hagar's blues / J. Tim Brymn, W.C. Handy (4:57) -- Long gone (from Bowlin' Green) / Chris Smith, W.C. Handy (5:08) -- The Memphis blues (or Mister Crump) / George A. Norton, W.C. Handy (2:59) -- Beale Street blues (4:56) -- Ole Miss Blues / W.C. Handy, Walter Hirsch (4:56) -- Chantez les bas (Sing 'em low) (4:48)...
Format: sound recording-musical
Publisher / Publication Date: Columbia/Legacy 1997
2 available in Compact Audio Disc, Call number: CD JAZZ ARM
Beauty is a rare thing : the complete Atlantic recordings
Coleman, Ornette.
Contents: Disc 1. Focus on sanity (6:49) -- Chronology (6:04) -- Peace (9:02) -- Congeniality (6:44) -- Lonely woman (4:57) -- Monk and the nun (5:53) -- Just for you (3:51) -- Eventually (4:20) -- Una muy Bonita (5:59) -- Bird food (5:28) -- Change of the century (4:41) -- Music always (5:29) -- Disc 2. The face of the bass (6:55) -- Forerunner (5:13) -- Free (6:20) -- The circle with a hole in the...
Publisher / Publication Date: Rhino Records 1993
Cross country tour, 1958-1961
Jamal, Ahmad.
Contents: But not for me -- Surrey with the fringe on top -- Moonlight in Vermont -- Music! Music! Music! (Put another nickel in) -- Woody 'n you -- Poinciana -- Too late now -- All the things you are -- Cherokee -- It might as well be spring -- I'll remember April -- Gone with the wind -- Billy boy -- It's you or no one -- You don't know what love is -- Tater pie -- This can't be love -- Old devil moon...
Publisher / Publication Date: GRP Records 1998
1 available in Compact Audio Disc, Call number: CD JAZZ JAM
Lady in satin
Contents: I'm a fool to want you (edited master, CS 8048) / J. Wolf ; J. Herron ; F. Sinatra (3:23) -- For heaven's sake / S. Edwards ; E. Bretton ; D. Meyer (3:26) -- You don't know what love is / D. Raye ; G. DePaul (3:48) -- I get along without you very well / H. Carmichael (2:59) -- For all we know / J.F. Coots ; S. Lewis (2:53) -- Violets for your furs / Adair ; Dennis (3:24) -- You've changed / M....
3 available in Compact Audio Disc, Call number: CD VOCAL HOL
Mingus ah um
Mingus, Charles
Summary: Program notes inserted in container.
1 available in Compact Audio Disc, Call number: CD JAZZ MIN
Super-sonic jazz
Sun Ra.
Contents: India (4:49) -- Sunology (5:40) -- Advice to medics (2:02) -- Super blonde (2:35) -- Soft talk / Julian Priester (2:41) -- Sunology part II (7:05) -- Kingdom of not (5:32) -- Portrait of the living sky (1:48) -- Blues at midnight (6:30) -- El is a sound of joy (3:56) -- Springtime in Chicago (3:51) -- Medicine for a nightmare (2:25).
Publisher / Publication Date: Evidence 1991
1 available in Compact Audio Disc, Call number: CD JAZZ SUN
Sarah Vaughan, 1951-1952.
Vaughan, Sarah
Contents: Ave Maria (3:27) -- City called heaven (3:30) -- Deep purple (3:07) -- These things I offer you (2:58) -- Vanity (2:35) -- My reverie (2:33) -- Out o' breath (2:37) -- After hours (2:50) -- Just a moment more (3:19) -- Pinky (2:42) -- I ran all the way home (3:10) -- Miracle happened (3:18) -- Street of dreams (3:01) -- Time to go (2:59) -- Corner to corner (2:58) -- If someone had told me...
Publisher / Publication Date: Classics Records 2003
1 available in Compact Audio Disc, Call number: CD VOCAL VAU
Art Blakey & the Jazz Messengers live in '58
Blakey, Art
Summary: One of the finest lineups in the history of jazz - Bobby Timmons, Jymie Merritt, Benny Golson, and the legendary trumpet player, Lee Morgan. This historic concert, filmed in Belgium in 1958, is the only known visual of this influential band.
Format: moving image
Publisher / Publication Date: Reelin' in the Years Productions 2006
1 available in Music DVDs, Call number: DVD MUSIC ART
Flautista! : Herbie Mann plays Afro-Cuban Jazz.
Mann, Herbie
Contents: Todos locos -- Cuban patato [sic] chip -- Come on, mule -- The Amazon River -- Caravan -- Delilah -- Basin Street Este.
Publisher / Publication Date: Verve 1998
1 available in Compact Audio Disc, Call number: CD JAZZ MAN
Brubeck & Rushing : the Dave Brubeck Quartet featuring Jimmy Rushing
Contents: There'll be some changes made / B. Higgins, B. Overstreet (2:07) -- My melancholy baby / G.A. Norton, M.E. Watson, E. Burnett (3:59) -- Blues in the dark / C. Basie, J. Rushing (4:39) -- I never knew (I could love anyone like I'm loving you) / T. Pitts, R. Egan, R. Marsh (2:29) -- Ain't misbehavin' / A. Razaf, T. Waller, H. Brooks (3:22) -- Evenin' / M. Parish, H. White (4:11) -- All by myself...
Publisher / Publication Date: Columbia Legacy 1998
1 available in Compact Audio Disc, Call number: CD JAZZ BRU
Blue hour : the complete sessions
Turrentine, Stanley.
Contents: I want a little girl / B. Moll, M. Mencher (7:02) -- Gee baby, ain't I good to you / D. Redman, A. Razaf (5:20) -- Blue riff / Gene Harris (6:25) -- Since I fell for you / Buddy Johnson (8:46) -- Willow weep for me / Ann Ronnell (9:55) -- Blues in the closet / Oscar Pettiford (4:59) -- Just in time / Styne, Comden, Green (5:40) -- Gee baby, ain't I good to you (alt tk) (5:31) -- Where or when /...
Publisher / Publication Date: Blue Note 2000
Jazz day : the making of a famous photograph
Orgill, Roxane
Summary: A collection of poems recounts the efforts of Esquire magazine graphic designer Art Kane to photograph a group of famous jazz artists in front of a Harlem brownstone.
Publisher / Publication Date: Candlewick Press 2016
1 available in Juvenile Nonfiction, Call number: J 811 ORG
Beverly Kenney sings with Jimmy Jones and "The Basie-ites."
Kenney, Beverly
Contents: Nobody else but me -- The more I see you -- Old buttermilk sky -- I never has seen snow -- A fine romance -- Who cares what people say -- Makin' whoopee -- The charm of you -- Isn't this a lovely day -- Mairzy doats -- My kind of love -- Can't get out of this mood.
Publisher / Publication Date: Fresh Sound Records 1989
1 available in Compact Audio Disc, Call number: CD VOCAL KEN
Dizzy's diamonds : the best of the Verve years
Contents: Disc I. Prelude / Schifrin (5:54) -- 'Bout to wail / Gillespie ; arr. by Buster Harding (6:46) -- Umbrella man / Larry Stock ; James Cavanaugh ; Vincent Rose (3:00) -- The chains / Schifrin (9:09) -- Birk's works / Gillespie ; arr. by Ernie Wilkins (4:56) -- Stella by starlight / Victor Young ; Ned Washington (4:05) -- Dizzy's business / Wilkins ; arr. by Wilkins (3:36) -- Autumn leaves /...
1 available in Compact Audio Disc, Call number: CD JAZZ GIL
East of the sun : the west coast sessions
Getz, Stan
Contents: Disc 1. Four / Miles Dewey Davis III (7:32) -- Split kick / Horace Silver (7:53) -- East of the sun (and west of the moon) / Brooks Bowman (6:17) -- A night in Tunisia / John Birks "Dizzy" Gillespie, Frank Paparelli (6:09) -- Suddenly it's spring / Jimmy Van Heusen, Johnny Burke (6:56) -- Summertime / George Gershwin, Ira Gershwin (6:04) -- S-h-i-n-e / Ford Dabney, Lew Brown, Cecil Mack (8:54)...
1 available in Compact Audio Disc, Call number: CD JAZZ GET
Count Basie swings, Joe Williams sings.
Basie, Count
Contents: Every day I have the blues.--The comeback.--All right, ok, you win.--In the evening (when the sun goes down.--Roll 'em Pete.--Teach me tonight.--My baby upsets me.--Please send me someone to love.--Ev'ry day (I fall in love).--As I love you.--Stop! don't.--Too close for comfort.
Publisher / Publication Date: New York, NY 0000
1 available in Compact Audio Disc, Call number: CD JAZZ BAS
A life in time : the Roy Haynes story.
Haynes, Roy.
Contents: Disc one (1949-1962): Ding dong (2:29) -- Bouncin' with Bud (3:04) -- My little suede shoes (3:06) -- Morpheus (2:22) -- Down (2:52) -- I know (2:32) -- I'll walk alone (4:57) -- Shulie-a-bop (2:41) -- Two brothers (3:32) -- How high the moon (2:37) -- Reflection (4:24) -- Rhythm-a-ning (9:25) -- Don't go to strangers (3:49) -- On Green Dolphin Street (5:45) -- I'm late, I'm late (45 rpm issue)...
Publisher / Publication Date: Dreyfus Jazz 2007
1 available in Compact Audio Disc, Call number: CD JAZZ HAY
Smithsonian collection of classic jazz, vol. 4 IV.
Contents: Boplicity / Miles Davis (Miles Davis and his orchestra) --Subconscious Lee / Lee Konitz (Lennie Tristano Ouintet) -- Body and soul / Johnny Green (Gene Norman's "Just Jazz" featuring Red Norvo and Stan Getz) --All alone / Irving Berlin (Sarah Vaughan) -- My Funny valentine / Richard Rodgers (Sarah Vaughan) -- Misterioso ; Evidence / Thelonious Monk (Thelonious Monk Quartet) -- Criss-cross /...
Publisher / Publication Date: Smithsonian Collection of Recordings 1987
2 available in Compact Audio Disc, Call number: CD JAZZ SMI
Best of Louis Armstrong
Armstrong, Louis
Contents: What a wonderful world -- Hello Dolly! -- Dream a little dream of me -- Cabaret -- That lucky old sun -- I still get jealous -- Blueberry hill -- A kiss to build a dream on -- Gone fishin' -- When it's sleepy time down south.
Publisher / Publication Date: MCA Records 1999
1 available in Compact Audio Disc, Call number: CD PM Armstrong
Ellington, Duke
Contents: disc 1 : It don't mean a thing (if it ain't got that swing) (Ivie Anderson) -- I'm satisfied (Ivie Anderson) -- I've got to be a rug cutter (Ivie Anderson) -- Swingtime in Honolulu (Ivie Anderson) -- You gave me the gate (and I'm swingin') (Ivie Anderson) -- I want something to live for (Jean Eldridge) -- A lonely coed (Ivie Anderson) -- Killing myself (Ivie Anderson) -- Love you madly (Yvonne)...
Publisher / Publication Date: Columbia Music Collection 1990
1 available in Compact Audio Disc, Call number: CD JAZZ ELL
Stormy weather : the legendary Lena, 1941-1958
Horne, Lena.
Contents: You're my thrill -- Good-for-nothin' Joe -- Love me a little little -- Don't take your love from me -- Stormy weather -- What is this thing called love? -- Ill wind -- The man I love -- Where or when -- I gotta right to sing the blues -- Moanin' low -- I didn't know about you -- One for my baby (and one more for the road) -- As long as I live -- I ain't got nothin' but the blues -- How long has...
Publisher / Publication Date: Bluebird 1990
1 available in Compact Audio Disc, Call number: CD VOCAL HOR
Art Tatum : 20th century piano genius.
Tatum, Art
Contents: Just like a butterfly -- Tenderly -- I cover the waterfront -- Body and soul -- Someone to watch over me -- In a sentimental mood -- Yesterdays -- Willow weep for me -- Wrap your troubles in dreams -- Makin' whoopee (incomplete) -- Memories of you -- September song -- Begin the beguine -- I'll never be the same -- Over the rainbow -- Love for sale -- My heart stood still -- Sweet Lorraine --...
Publisher / Publication Date: Jazz Heritage 1997
1 available in Compact Audio Disc, Call number: CD JAZZ TAT
Howard McGhee. Introducing the Kenny Drew Trio.
McGhee, Howard
Contents: Meciendo -- Lo-flame -- Fluid Drive -- I'll remember April -- Fuguetta -- Donnellon Square -- Lo-flame (alt. tk.) -- Yesterdays -- Stella by starlight -- Gloria -- Be my love -- Lover come back to me -- Everything happens to me -- It might as well be spring -- Drew's blues -- Yesterdays (alt. tk.) -- Everything happens to me (alt. tk.).
1 available in Compact Audio Disc, Call number: CD JAZZ MCG
Tristano, Lennie.
Contents: Smog eyes (3:32) -- Ear conditioning (5:13) -- Lover man (4:28) -- Quintessence (4:14) -- Jazz of two cities (4:32) -- Dixie's dilemma (4:20) -- Tschaikovsky's opus #42, third movement (3:59) -- I never knew (5:00) -- Ear conditioning (mono. master) (5:14) -- Lover man (mono. master) (4:29) -- Jazz of two cities (mono. take) (4:39) -- I never knew (mono. take) (5:09) -- Wow (3:19) --...
Publisher / Publication Date: Capitol Jazz 1996
1 available in Compact Audio Disc, Call number: CD JAZZ TRI

redpajama_set_name: RedPajamaCommonCrawl


text:
WE ARE OFFICIALLY BACK IN FULL SWING! / / FLAT RATE SHIPPING $11.95 AUS WIDE // AFTERPAY AVAILABLE.
Just For Our Babies
Constructive & Small World Play
Reading & Learning Corner
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Home / Products / Atlas of Ocean Adventures
About
From the team behind the best-selling Atlas of Adventures comes the deepest adventure yet - a trip through the oceans of the world to discover creatures of the deep and see the unique environments in which they live.
Set your spirit of adventure free with this journey to the world's great oceans, discovering the diversity of life that exists in the deep blue sea. Whether you're travelling long haul with leatherback turtles across the Pacific, snoozing with sea otters or ice bathing with a walrus, this book celebrates the very prescient topic of the world's oceans with Lucy Letherland's animal characters. A natural history lesson in an adventure book, each spread features 10 captions and and facts about every destination. The 5th title in the best-selling Atlas of Adventures series that has now been translated into 31 languages.
Emily Hawkins is a writer and editor of children's books for all ages. She wrote the New York Timesbestseller Oceanology, as well as several other titles in the Ology series, which has sold over 16 million copies worldwide. She holds a first-class English degree from Nottingham University, and now lives in Winchester with her young family.
About the Illustrators
Lucy Letherland is an illustrator based in London, UK. She graduated from Manchester School of Art in 2011 with a First Class BA (Hons) in illustration with animation. Lucy's work is strongly led by humour and narrative, creating a playful, graphic quality. Her books include Atlas of Adventures, Atlas of Adventures: Wonders of the World, Atlas of Animal Adventures and Atlas of Dinosaur Adventures.
Online Store: Always Open!
hello@thecuratedparcel.com


text:
We're still the kings of Manchester, insists Solskjaer
Ole Gunnar Solskjaer says the rebuilding work at Manchester United will take time.PHOTO: REUTERS
MANCHESTER CITY MANCHESTER UNITED
Manchester City may have won back-to-back English Premier League titles, and currently stand 11 points clear of Manchester United, but Ole Gunnar Solskjaer insists his team are still bigger than their neighbours.
Despite not winning a championship since 2013, the Old Trafford boss insists his side are the biggest – and will one day return back to the top.
"As a club, the size of our club, we're going to have to bridge that gap and our aim is to go past the teams above us and I believe at Man United that's what we have to aim for, that's what we have to go for and that's what we have to believe in," said Solskjaer who faces City in a Manchester Derby on Sunday morning (Singapore time).
"We have the resources to do it, we have the people to do it, so why not?"
Solskjaer mocked City's past struggles as he recalled a five-year wait before playing in a Manchester Derby.
The Norwegian joined United in the summer of 1996 just after City had been relegated to the second tier – and eventually faced them in a 1-1 draw in 2001.
"At least we play every year now," he added.
"Took many years before I played a Manchester Derby myself, it's changed in a way."
And when asked if United were still bigger, despite City's recent dominance, he responded: "Yeah." Solskjaer also dismissed the views of former bosses David Moyes and Jose Mourinho that City's spending power meant United would always struggle to match them.
"Don't agree," he added. "What are you going to do? Are you going to give up? Not challenge them? That's what we've got to get back to.
"How? Don't deviate from a plan that you have set out and believe in what we're doing behind the scenes, believe in the players, believe in the coaching staff.
"As long as we're going in the right direction and we get there, that day when we do it is going to be a very good day."
Solskjaer said United would also look to strike the right balance in their squad with their transfer strategy.
"Do I look like I'm going to spend hundreds of millions of pounds on players we're not sure of?" he said.
"As I said, we need to rebuild. We need to change the culture, you want the culture with that hunger and selflessness that most of these players are showing.
"You've got the (Scott) McTominays and (Marcus) Rashfords and (Jesse) Lingards, the players that know what Man United is.
"We keep on going in the direction we're going. We know we need to strengthen the squad in depth."
Having beaten Chelsea, Leicester and Tottenham, and drawn with Liverpool, this season, Solskjaer says City will hold no fears for his side when they go to the Etihad.
"They haven't had the results of last year, but they're still the best team in the league when they're playing the way they can," he added.
"You can't argue we're too far behind, but it's a chance for us now to challenge them and bridge that gap a little bit."
Rashford hits double as Man United thrash Norwich 4-0
Anthony Martial returns to the squad after missing the Spurs game, but Paul Pogba remains sidelined following his ankle injury. – AFP
Ole Gunnar SolskjaerManchester Unitedmanchester city


It looks beautiful. I hope we get to paddle together there sometime. It's been a while. I was thinking of you and I and Clover going down the Skeena after your earlier post. I agree wholeheartedly…more coffee and paddling. And it was great to hear your voice on the clip!


The wealth of this country lies in its people––not in its possessions, but in its people.
Government only exists for the sake of the people. It may not subject the rights of any person to another. It may not endorse slavery. It may not order, or sanction, or permit, or assist, the killing of any of its innocent members.
There is no doubt of the humanity of the unborn child from the moment of conception. From that moment, each human being (and in this he differs from brute animals) is invested with a spiritual soul by which is constituted the human person. Nothing is added to the conceptus thereafter but nutrition, time and the opportunity to develop. Abortion, at any stage of gestation involves, therefore, the killing of a human person.
No one with a rightly formed conscience could vote in favour of abortion, or vote to tolerate its continuance on the statute books.
That any government, State or Federal, should legislate so as to allow abortion, or fail to enforce a law prohibiting it, is reprehensible. Any politician, from Prime Minister or Premier down, who acts in this way, or condones such action, deserves ongoing public condemnation.
Far from facilitating the use by its citizens of the facilities of abortion clinics, government, both State and Federal, should act so as to remove the incentives for them to do so including, where necessary, providing essential financial assistance.
Abortion should be removed from the schedule of medical benefits under Medicare. It is grossly unjust that the taxes of Australia's citizens should be applied to fund the killing of the innocent unborn.
Crimes such as abortion cry to heaven for vengeance. The systematic condoning of abortion constitutes a curse on this great country which affects, even now, all its citizens. It is inevitable that the consequences of this great evil will be felt more and more unless action is taken to remove it and reparation is made to Almighty God for the grave sins involved.
All this being said, there is no sin which Almighty God cannot forgive, provided only that the sinner acknowledges his sin and seeks His forgiveness. Every priest of the Catholic Church throughout the country who has faculties from a bishop of this Conference, is available to see and to discuss with any person, whether Catholic or not, in complete confidence, issues of conscience in this matter of abortion that are troubling him. Such a priest has the power, moreover, if the person involved is baptised, to hear his confession and to give him absolution.
There should be established throughout the country in every diocese a systematic program of Masses, of adoration of the Blessed Eucharist, of prayers and penance on the first Saturday of each month and the Sunday following for the ending of this curse. Each bishop of this Conference will put in place in his diocese such a program.
This Conference intends that there should be established a shrine of reparation to Almighty God for the sins of abortion committed throughout the country similar to the basilica, Sacre Coeur, in France. The bishops will give consideration to establishing such a shrine and where it will be established.
This Conference notes that this evil of abortion is allied, as effect to cause, to the contraceptive mentality which dominates Australian society and will speak on this subject more fully hereafter.
This Conference notes further that in vitro fertilisation, which involves the medical interference in human procreation, and the abuse of the fertilised human embryos which the process produces, and the further abuse and destruction of these fertilised human embryos in embryonic stem cell research, are a gross interference in the rights of Almighty God. Again this is a subject on which this Conference will speak further and more fully hereafter.


I've managed to find one of these, but does anyone have a pic of how they attach to the bike?
Hi, I think they go onto the main engine / body bolt. I think they will fold down to be used and flip up when out of use.


Remember that neat little printable bug craft from a couple months ago?
I thought the bug templates I made were so fun, I knew I had to come up with a way to use them again. So I made a little game for the boys. And I know how much you all love printable crafts and activities, so I'm sharing it with you today.
You can download the free printable bug jump game here when you sign up for my free library of printable crafts. I'll send you a link to a secret page where you can download all my fun freebies.
Print it the bug jump game. I used cardstock for this game, but regular paper would work also.
You can either leave the craft blank or color the bugs interesting colors. My boys chose to leave the bugs blank to play this time around.
Assemble the game using the instructions. Using the glue tabs, glue the long jump path together.
Place the bugs on the 'Start' and see how far you can jump them.
The boys had fun jumping them several times to reach the end of the path.


text:
O marketing de Wario Land: Shake It!, jogo eletrônico de 2008 para Wii, foi composto por diversas campanhas, sendo a mais notável um vídeo no YouTube no qual o protagonista Wario realiza várias ações de grande impacto e coleta itens, fazendo com que a página ao redor fique destruída pouco a pouco enquanto esses itens se acumulam ao redor a página. O vídeo foi dirigido por uma equipe da empresa de marketing Goodby, Silverstein & Partners e produzido por Jennifer Wilson da produtora Mike Kellogg.

O vídeo acabou sendo retirado do ar e substituído por um anúncio em estilo documentário para o jogo Punch-Out!!, criado pela mesma empresa. O anúncio teve sucesso entre os usuários do YouTube, jornalistas e profissionais de marketing, obtendo 4 milhões de visualizações apenas no primeiro mês, e recebeu diversos reconhecimentos, principalmente por inspirar futuros anúncios de outras empresas.

Vídeo
O anúncio do YouTube apresenta a jogabilidade do jogo eletrônico Wario Land: Shake It!, mostrando Wario passando por várias partes do jogo. Ao longo do vídeo, vários impactos ocorrem, fazendo elementos ao redor da página cair (como vídeos recomendados, descrições de vídeos e outras funções do YouTube). Moedas e outros objetos também saem de dentro do vídeo e se espalham pela página. O vídeo termina com o logotipo do jogo caindo em cima do mesmo, fazendo com que o vídeo caia sobre uma pilha de elementos da página. Os visualizadores podiam pegar os elementos que caíam pela página com o cursor, arrastando-os e soltando-os.

História
O trailer foi lançado em 2008 como um dos primeiros vídeos interativos do YouTube. Seus diretores criativos foram Jeff Goodby e Rich Silverstein da empresa de marketing Goodby, Silverstein & Partners. A direção de arte ficou a cargo de Bryan Houlette, cujo assistente de direção de arte foi Erik Enberg. Foi produzido pela Mike Kellogg, e seu produtor foi Jennifer Wilson. O vídeo foi criado para o YouTube em parte devido à percepção de que o YouTube é o lugar onde as crianças podem ir para ver vídeos de jogos eletrônicos. A destruição da página ao redor foi feita com o anúncio deste jogo porque refletia a natureza destrutiva de Wario. O YouTube foi inicialmente cético em relação a um anúncio que destruía seu site, mas acabou mudando de ideia devido a seu aparente mérito criativo e de marketing. O anúncio foi removido do YouTube e substituído por um anúncio no estilo documentário para Punch-Out!!, criado pela mesma equipe de marketing por trás do anúncio de Shake It!.

A campanha foi criada para atrair adolescentes e teve um orçamento de 80 mil dólares. A Nintendo também realizou uma competição num parque de diversões Six Flags perto de Los Angeles, onde competidores competiram por um "saco de moedas sem fundo". Os participantes receberam bigodes falsos de Wario, e o vencedor ganhou o saco e uma viagem com todas as despesas pagas para o Nintendo World em Nova Iorque. Outra campanha de marketing teve a Nintendo dando gasolina em uma Mobile Gas, em Los Angeles, para comercializar Shake It!, em referência à flatulência de Wario.

Recepção
O anúncio do YouTube foi bem recebido por jornalistas, usuários do YouTube e profissionais de marketing. A campanha foi bem-sucedida com esse grupo demográfico, atingindo 24% de reconhecimento com uma meta inicial de 12-15%. O anúncio chamou muita atenção, acumulando 4 milhões de visualizações no primeiro mês. Foi o primeiro anúncio desse tipo, gerando anúncios semelhantes nos meses seguintes. Apesar da recepção positiva, o anúncio não conseguiu impulsionar as vendas do jogo para atingir o número pré-objetivo de 350 mil unidades até o final de 2008, o que a equipe de campanha atribuiu a uma economia fraca e vendas baixas de jogos em geral. Um representante do YouTube disse à equipe por trás do anúncio que isso fez com que eles recebessem várias ligações de anunciantes questionando por que essa função não era conhecida por eles. Os autores Damian Ryan e Calvin Jones discutiram o anúncio do YouTube como um estudo em marketing, enquanto o elogiavam por sua inovação. Ele recebeu um prêmio de prata na 88ª edição anual da "The Art Directors", enquanto o diretor de arte Robert Lindstrom elogiou o anúncio do YouTube por chamar a atenção para Shake It! De uma forma única. O comerciante e autor Avinash Kaushik chamou-o de "criativo" e afirmou que adorou o anúncio.

O escritor da Kotaku Mike Fahey elogiou o "gênio" do anúncio no YouTube ao compará-lo favoravelmente com a campanha de distribuição de gasolina da Nintendo, que ele considerou "obsoleta". Um escritor da GameZone expressou tristeza com a remoção do anúncio, pois, a partir dali, seria possível vê-lo apenas através de vídeos não interativos do YouTube. Ele considerou o vídeo o melhor anúncio da Nintendo de todos os tempos. A escritora da Destructoid Colette Burnett sentiu que o anúncio seria memorável para seus espectadores. Burnett, junto com o escritor da Wired Chris Kohler e o escritor da Joystiq Ross Miller, consideraram-no um anúncio inteligente, com o último elogiando-o como um "surpresa divertida." O escritor da CNET Josh Lowensohn elogiou-o como "memorável" e "incrivelmente legal", afirmando que o anúncio colocaria um "sorriso no rosto [dos espectadores]".

Notas

Vídeos do YouTube
Campanhas publicitárias
Marketing de jogos eletrônicos
Wario
Wii

redpajama_set_name: RedPajamaWikipedia


Focus Hub Nigeria is organizing the maiden edition of #GirlsinICT Hangout with Ese Emerhi and Sharon D. Fiberesima on November 8, 2014 at Grand Venice Hotel, Cocaine Village, 1st Artillery, Port Harcourt at 12 noon.
The Niger Delta Development Forum (NDDF) is a unique advocacy platform that informs and influences promotion of non-oil pro-poor policies, programs and interventions as well as leverage and advice on how resources from the public, private and development organizations can be effectively and efficiently utilized to promote inclusive and equitable economic growth.
The Ondo State governor, Dr Olusegun Mimiko, has inaugurated the "Lakwa Vanguard", a youth empowerment scheme initiated for the youth of the riverine communities of the state.
The State Employment and Expenditure for Result (SEEFOR) Project has employed 1,226 youths in Bayelsa State in the area of road maintenance and sanitation under its public works component.
The Abia State Governor, Theodore Orji, has commissioned new 'model schools' in the state.
The Coordinator of State Employment and Expenditure for Results programme of the Delta State Government, Mr Benson Ojoko, said the project had trained 524 youths on refuse disposal.
Edo State Government has said that the state would continue to maintain her polio free status as no case of polio has been recorded in the state since March, 2009.
The United Nations Industrial Development Organization, UNIDO and the Foundation for Partnership Initiatives in the Niger Delta, PIND have signed a Memorandum of Understanding on poverty reduction through productive activities in the Niger Delta.
ONDO State Wealth Creation Agency (WECA) in conjunction with Ministry of Commerce and Industry and Middleman Incorporation has organised the first Made in Ondo Fair to sensitise local business owners on how to avail public opportunities to empower themselves economically and create more wealth for the nation.


http://thedook.com/365/wp-content/uploads/2013/01/red_or_blue_pill.jpg 1330 2000 Cathy Neth http://thedook.com/365/wp-content/uploads/2016/04/facebookpreviewphoto.jpg Cathy Neth2013-01-08 18:23:112015-01-24 14:18:27Red or Blue?
7/365: Standout Standout in a crowd. Be unique. Be an individual. Be you!
2/365: Blast Off Legos Ready to blast off into 2013.
328/366: Helper We all need helpers sometimes in life. Skippy is a great helper when working on puzzles.
311/366: Halo 4 Got my copy of Halo 4 and I'm ready to start playing! Best FPS game series ever.
289/366: Happy Birthday! Celebrating on a beautiful day.
http://thedook.com/365/wp-content/uploads/2012/10/happy_birthday_cathy.jpg 1968 3264 Cathy Neth http://thedook.com/365/wp-content/uploads/2016/04/facebookpreviewphoto.jpg Cathy Neth2012-10-15 14:53:422015-01-24 13:24:36Happy Birthday!
282/366: Eco Lunchbox Save the earth, use less plastic and go Eco Lunchbox.
234/366: Shoes Optional Where the toes meet the sand, shoes are optional.
185/366: Happy Feet III Sanuks: Helping navigate life one step at a time.
180/366: Happy Feet II There are 2 things in this photo that make me very happy. My Sanuks and my ducks. Happy feet II.
140/366: Happy Birthday Dad To the best dad - Happy Birthday dad. Thanks for all you do.
21/366: Lego Land Leave Your Mark Wherever you go leave your mark, leave your influence, leave your best.
19/366: Industry in the Morning Industry is just walking up, the train bells ring and the sirens shout. Wake up wake up.


Business Continuity is becoming ever more critical and in today's cloud world should be easier. Yet in recent hits of bad weather, 'The Beast From The East' had an impact. Users should be tied to their phone numbers, but not tied to the physical device or location.


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text:
Home INDIA & BEYOND MH370 hunt: Australian aircraft detects possible signal
MH370 hunt: Australian aircraft detects possible signal
Canberra, April 10:
A Royal Australian Air Force (RAAF) AP-3C Orion aircraft has detected a possible signal consistant with the missing jet in the vicinity of the Australian Defence Vessel (ADV) Ocean Shield, an official confirmed Thursday.
"The acoustic data will require further analysis overnight but shows potential of being from a man-made source," said Angus Houston, chief coordinator of the Joint Agency Coordination Center (JACC).
Pic source : berberanews.com
Joint Agency Coordination Center (JACC) is leading the multi-national operation to search for the missing Malaysian Airlines jetliner that vanished mysteriously with 239 on board.
According to JACC figures, the ADV Ocean Shield is narrowing down Thursday's search area from 75,000 square km to 57,923 km, which lies approximately 2,280 km northwest of Perth, Xinhua reported.
The ADV Ocean Shield detected four signals Saturday and Sunday.
"Hopefully with lots of transmissions we'll have a tight, small area and hopefully in a matter of days we will be able to find something on the bottom that might confirm that this is the last resting place of MH370," Houston was quoted as saying.
Up to 14 planes and 13 ships have joined in Thursday's search for the missing Malaysia Airlines flight MH370.
Except for the search operation on the ocean surface, the underwater search also continued Thursday, with the Ocean Shield at the northern end of the defined search area, and Chinese ships Haixun 01 and HMS Echo at the southern end.
Two separate signals were detected Sunday by a US pinger locator being towed by the ADV Ocean Shield in the Indian Ocean search area, about 1,700 km northwest of Perth.
The first detection of the signal lasted for two hours and 20 minutes. After few hours, the second signal was detected which lasted for 13 minutes.
The two signals were about 1800 metres apart.
The ADV Ocean Shield detection Sunday came shortly after a Chinese patrol vessel, the Haixun One Zero, reported detecting two pulse signals Friday night, and then again Saturday at a frequency consistent with black box technology.
The Malaysia Airlines flight MH370 vanished mysteriously about an hour after taking off for Beijing from Kuala Lumpur shortly after midnight March 8.
The Boeing 777-200ER was scheduled to land in Beijing the same day. The 227 passengers on board included five Indians, 154 Chinese and 38 Malaysians.
Despite extensive scouring of the remote southern Indian Ocean area by planes and ships off the coast of Perth, where the plane is believed to have crashed, no trace has been found.
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Next articleOdisha polls: Tathagata in for toughest fight of career in Dhenkanal


Earned the 99 Bottles (Level 39) badge!
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Earned the Photogenic Brew (Level 13) badge! Earned the Draft City (Level 39) badge! Earned the Wheel of Styles (Level 26) badge! Earned the Heavy Weight (Level 9) badge!
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Famous sign from California. Price includes shipping and insurance, contact us to discuss if you wish.
These are not photos of the actual storefronts! Hage constructs 1:12 scale models by hand, then makes prints of the original model (which sell for 18-25k).
We also have a 3 1/4 x4 1/4 framed, matted 9x11" print for $125.00.
These are not photos of the actual storefronts! Hage constructs 1:12 scale models by hand, then makes prints of the original model (which sell for 18-25k). Free shipping!
Owned by JJ Abrams, this was his grandfather's store in the lower east side of NY.


text:
\section{Introduction}
\noindent
The relationship between gas-rich late-type dwarfs---irregulars and blue compact dwarfs (BCDs)---and early-type dwarfs---dwarf ellipticals and spheroidals---is unclear. Are late-type dwarfs the progenitors of early-types, or are the two populations largely distinct, with late-types evolving in the field and dwarf ellipticals in cluster environments? On one hand, many early-type dwarfs show late-type features: faint disk-like structures (\citealt{Lisker2006disk}; \citealt{Penny2014}), rotational support (\citealt{Beasley2009}; \citealt{Guerou2015}; \citealt{Toloba2016}), and lingering central star formation (\citealt{Lisker2006bc}; \citealt{DeLooze2013}). In turn, the underlying old stellar population of late-type dwarfs resemble dwarf ellipticals and spheroidals (\citealt{Meyer2014}). On the other hand, simulations (\citealt{Weinmann2011}; \citealt{Lisker2013}; \citealt{Mistani2016}) and stellar population modeling (\citealt{Rakos2004}; \citealt{Koleva2009}; \citealt{Paudel2010}; \citealt{Roediger2011}; \citealt{Weisz2014}; \citealt{Guerou2015}) suggest that early-type dwarfs essentially halted star formation at $z\sim1$, and so late-type dwarfs at $z=0$ are unlike their progenitors.

Essentially all dwarfs in the field are star-forming or in a starburst phase (\citealt{Lee2009}; \citealt{Geha2012}) while quiescent dwarf ellipticals predominate in the cluster (\citealt{Dressler1980}; \citealt{Binggeli1987}). If these populations are related, then it is assumed that the cluster environment is responsible for this transformation. As gas-rich late-type galaxies fall onto the cluster, their gas is removed via processes such as ram-pressure stripping (\citealt{Boselli2008}; \citealt{Boselli2016}) or galaxy harassment (\citealt{Mayer2001}; \citealt{AguerriGonzalez2009}). This process is relatively rapid, less than 100 Myr (\citealt{Boselli2008}). By the time a dwarf galaxy has crossed through the cluster core, they are almost entirely gas free ($>99$\% gas removed). Without gas, star formation ceases, the galaxy's colors redden, and it loses any irregular or spiral features, becoming a smooth dwarf elliptical.

Given that gas removal precedes morphological changes, there should be few, if any dwarf elliptical galaxies which still have a detectable reservoir of \mbox{H\textsc{i}}. And indeed there are only a few, about 2\%, which do (e.g. \citealt{HuchtmeierRichter1986}; \citealt{diSeregoAlighieri2007}; \citealt{Taylor2012}). In the work of \citet{Hallenbeck2012}, hereafter H12, we identified a sample of 7 gas-bearing dwarf elliptical galaxies in the Virgo Cluster. The star formation in this sample is clearly suppressed: the galaxies are as red as typical dwarf ellipticals in the $g-i$, NUV$-r$, and FUV$-r$ bands. Additionally, their gas fractions ($GF\equiv M_\text{HI}/M_*$) are typical for unstripped dwarfs both in Virgo and the field \citep{Huang2012}. Based on this, we argued that the gas has been recently accreted.

How plausible is this assertion, given their evidence? Most dwarf ellipticals have cluster orbits which are highly radial \citep{Conselice2001}. This means that they will spend most of their time near the cluster edge---which is where the sample preferentially lies---where they can encounter clouds of neutral gas falling onto the cluster. {At their present positions outside the x-ray emitting region of Virgo, accretion is possible, as evaporation of clouds of neutral \mbox{H\textsc{i}}\ due to the hot intracluster medium is relatively slow compared with the time it would take to accrete a cloud of \mbox{H\textsc{i}}\ (H12).}

The purpose of this work is to test the re-accretion hypothesis of H12, using new deep optical and \mbox{H\textsc{i}}\ observations. In \S\ref{sec:sample}, we review and update the sample of H12, removing galaxies whose \mbox{H\textsc{i}}\ was not confirmed. In \S\ref{sec:results}, we present the results of new optical and \mbox{H\textsc{i}}\ observations of the sample. We weigh the evidence for morphological transformation of the galaxies in \S\ref{sec:morphology}, for recent accretion in \S\ref{sec:accretion}, and for quenched star formation without gas removal in \S\ref{sec:starburst}. In \S\ref{sec:gasstripping}, we argue that VCC 190 has had gas removed via tidal stripping.

\section{Sample Selection and Updates}
\label{sec:sample}
\noindent
Our sample selection is outlined in Table 1, as well as below. In H12, we defined a sample of dwarf elliptical galaxies in the Virgo cluster. These galaxies were identified using the morphology and subcluster assignments  from the Virgo Cluster Catalog (VCC; \citealt{Binggeli1985}), updates from \citep{Binggeli1993}, and our own internal assignments.

\begin{deluxetable}{lr}
\tablecolumns{2}
\tablewidth{0pt}
\tabletypesize{\scriptsize}
\tablecaption{Sample Counts}
\tablehead{
  \colhead{Selection Criteria} & \colhead{Galaxies}}
\startdata
Binggeli et al 1985 (VCC) Galaxies         & 2096\\
Dwarfs Ellipticals in Virgo                &  365\\
Red dEs with \mbox{H\textsc{i}}\ Detections (H12)         &    7\\
\mbox{H\textsc{i}}\ Confirmed by Follow-Up                &    5\\
Removal of VCC 956 and VCC 1993 (see text) &    3\\
\enddata
\tablecomments{\label{tab:sample-select}Number of galaxies in sample after each cut was applied. This work is concerned only with the 3 which remain after all cuts have been applied.}
\end{deluxetable}

Of these 365 dwarf ellipticals, 7 both had enough \mbox{H\textsc{i}}\ such that they were detected in the {Arecibo Legacy Fast ALFA survey (\nolinebreak{ALFALFA}; \citealt{Giovanelli2005}; \citealt{Haynes2011})} and clearly lay along the red sequence (SDSS $g-r\geq0.45$).

\subsection{ALFALFA Follow-Up}
\noindent
The \mbox{H\textsc{i}}\ detections of this sample were often near the detection limit of \nolinebreak{ALFALFA's}, with signal-to-noise ratios of $3<SN<10$. So, we re-observed the each object as part of a larger ALFALFA campaign to confirm the \mbox{H\textsc{i}}\ in unusual and low signal-to-noise galaxies.

We performed a 3 minute ON/OFF observation of each galaxy using the single pixel L-Band Wide (LBW) receiver. These pointed observations have an rms of 1.1 mJy in 10 km~s$^{-1}$\ wide channels, and are thus twice as sensitive as ALFALFA, which has a typical rms of 2.2 mJy when smoothed to the same width.

Out of the seven, the \mbox{H\textsc{i}}\ emission in five of the galaxies was confirmed. The two galaxies with the lowest signal-to-noise (VCC 421 and VCC 1649) were not confirmed, and so we remove them from our sample.

\subsection{The Trouble With VCC 956 and VCC 1993}

\citet{OosterloovanGorkom2005} mapped an \mbox{H\textsc{i}}\ tail caused by ram-pressure stripping off of NGC 4388, which ranges in velocity from $2000<v<2600$ km~s$^{-1}$. The sky position of VCC 956 coincides with the end of the tail, as shown in Figure \ref{fig:vcc956-environment}. Our nominal \mbox{H\textsc{i}}\ detection has a velocity of $v=2200$ km~s$^{-1}$, which perfectly coincides with the velocity of NGC 4388's tail at that position (see \citealt{OosterloovanGorkom2005}, Figures 1 and 2). There are no independent redshift measurements of VCC 956. It is thus likely that our nominal \mbox{H\textsc{i}}\ measurement of VCC 956 is better identified with the tail of NGC 4388, and we remove it from our sample.

\begin{figure}[!ht]
\epsscale{1.15}
\plotone{fig-VCC956-environment.eps}
\caption{VCC 956 and its local environment. VCC 956 lies along the tidal tail off of NGC 4388, and our \mbox{H\textsc{i}}\ redshift coincides with the tail redshift of $2200$ km~s$^{-1}$. It is thus likely that the \mbox{H\textsc{i}}\ detected at the sky location of VCC 956 is not associated with the galaxy, and we remove it from our sample. Background is a DSS/II composite optical image, while contours are integrated \mbox{H\textsc{i}}\ flux from ALFALFA covering $1820$ km~s$^{-1}$ $<v<2630$ km~s$^{-1}$. Contours begin at $4\sigma$ (0.6 Jy km s$^{-1}$ beam$^{-1} = 0.1\ M_\odot$ pc$^{-2}$), and increase by a factor of $\sqrt{2}$ at each additional contour. The $3.8^{\prime}\times3.5^{\prime}$ ALFA beam is shown for reference.
\label{fig:vcc956-environment}}
\end{figure}

The surface brightness profile of VCC 1993 indicates that it is not a dwarf elliptical, but a low mass elliptical. It also has the highest $M_*$ in the sample by a factor of 10. So, we remove it from present consideration and focus on the lowest mass, truly dwarf, galaxies.

The remaining three galaxies, VCC 190, VCC 611, and VCC 1533 are the focus of this work.
\\
\section{Observations and Results}
\label{sec:results}
\subsection{Summary of Prior SDSS, GALEX, and ALFALFA Observations}
\label{sec:summary}
\noindent
Figure~\ref{fig:colors} (left) shows an NUV-r color-magnitude diagram of the dwarf sample of H12. Late-type dwarfs with \mbox{H\textsc{i}}\ are crosses, while early type dwarfs undetected in ALFALFA are gray dots. The three gas-rich dwarf ellipticals in our sample are plotted as red squares, and labelled with their VCC numbers. With a few exceptions, the late-type and early type dwarfs separate themselves neatly. From our sample, VCC 190 is unambiguously red in NUV$-r$ color. VCC 611 and VCC 1533 lie in the green valley; while they are redder than almost all of the late-type dwarfs, they are also bluer than most dwarf ellipticals. The galaxies show a similar segregation in FUV$-r$ and $g-r$ colors (see H12; Figure~6).

\begin{figure*}[ht]
\begin{center}
\epsscale{0.57}
\plotone{fig-colors.eps}
\plotone{fig-gasfraction.eps}
\end{center}
\caption{The 3 dwarf galaxies in our sample are red like typical dwarf ellipticals yet similar in gas richness to star-forming dwarf irregulars in the Virgo Cluster. (left) Ultraviolet and optical color-magnitude diagram of the dwarf galaxies in the Virgo Cluster. Crosses are late-type dwarfs with gas, gray circles are dwarf ellipticals without gas. Our sample of gas-bearing dwarf ellipticals are labeled with red squares. (right) Gas fraction as a function of stellar mass for late type dwarfs and our sample. Lines indicate the best fit and $2\sigma$ scatter for the late type dwarfs, and arrows are the $3\sigma$ upper limit for non-detected dwarf ellipticals based on stacking. All measurements are from \citet{Huang2012} with updates in H12.
\label{fig:colors}}
\end{figure*}

Figure~\ref{fig:colors} (right) shows the \mbox{H\textsc{i}}\ gas fraction as a function of stellar mass of late type dwarfs (crosses) along with a best-fit trend. The \mbox{H\textsc{i}}-bearing late-type dwarfs lie along the same line as \mbox{H\textsc{i}}-bearing dwarfs outside of the Virgo cluster (H12; \citealt{Huang2012}). This suggests that such galaxies have yet to undergo any significant stripping processes. Red boxes with labels are our sample. All three galaxies lie at or below the line defined by the HI-bearing late types, but none significantly so.

Arrows are 3$\sigma$ upper limits on the gas fractions of dwarf ellipticals which were not detected in ALFALFA derived from spectral stacking. The Arecibo Galaxy Environment Survey (AGES; \citealt{Auld2006}) found similar upper limits over a smaller region of the cluster (\citealt{Taylor2012}).

The three dwarf ellipticals in our sample thus fall into an unusual class: from their optical and ultraviolet magnitudes alone, they appear to fit in with the dwarf elliptical population by being either ``red and dead'' (VCC 190), or nearly so (VCC 611 and 1533). However, from their \mbox{H\textsc{i}}\ gas fractions, they appear to be unstripped late-type dwarfs, and several orders of magnitude more gas-rich than other dwarf ellipticals.

\subsection{Optical Observations}
\label{sec:optical}
\noindent
We obtained optical r-band imaging at the WIYN 0.9m telescope with the HDI camera at the Kitt Peak National Observatory (KPNO). VCC 190 and VCC 611 were observed for 30 and 36 minutes, respectively, with seeing $1^{\prime\prime}.6$. In addition, all three galaxies lay within the footprint of the Next Generation Virgo Survey (NGVS; \citealt{Ferrarese2012}), performed with the CFHT. All three galaxies were observed for between 30 minutes and 1 hour in the $u$, $g$, and $i$ bands.

Optical NGVS images of all three galaxies in our sample are shown in Figure~\ref{fig:sample} (top panels). The three galaxies all appear roughly elliptical but with some peculiar morphology. The highest optical surface density in VCC 190 (top left) is offset from the center, with possible tails to the west and south. The shape of VCC 1533 (right) is boxy, with a nucleated center. Figure~\ref{fig:sample} (second row) shows r-band (VCC 190 and 611) and i-band (VCC 1533) surface brightness profiles. All three galaxies are well-fit with an exponential profile for $r > 5^{\prime\prime}$ (dashed line), consistent with the standard dwarf elliptical profile. At smaller radii, the surface brightness profiles of VCC 1533 is contaminated by what is likely a foreground star.

VCC 611 (top center) appears like a smooth elliptical, likely due to its relatively higher stellar mass and surface brightness compared with the other two galaxies in our sample. However, it clearly has a very blue center indicative of star formation, which can be seen in Figure~\ref{fig:bluecenter}. The left panel presents an $i$-band image, which shows a smooth old stellar population. The right panel is a $g-i$ color map of the galaxy, which shows several star-forming knots in the galaxy's center. VCC 611 was observed as part of the SDSS spectroscopic survey and has H$\alpha$\ in emission with an equivalent width (EW) of 25 \AA \ (NASA Sloan Atlas\footnote{www.nsatlas.org}). \citet{Lisker2006disk} and \citet{Taylor2012} previously performed unsharp masking on all three of these galaxies using shallower SDSS images, but did not detect the underlying structure or the blue center in VCC 611.\\\\

\begin{figure*}[!htp]
\epsscale{1.1}
\plotone{fig-optical.eps}\\
\plotone{fig-profiles.eps}\\
\plotone{fig-spectra.eps}
\caption{Optical images and \mbox{H\textsc{i}}\ spectra of our sample of `red and dead' yet gas-bearing dwarf ellipticals. (top row) Optical CFHT images of the three red dwarf elliptical galaxies in the sample, using $u$-, $g$-, and $i$-band filters. (second row) Surface brightness profiles of the three galaxies; dashed lines are exponential profiles fit to $r > 5^{\prime\prime}$. (third row) \mbox{H\textsc{i}}\ Spectra; red dashed lines are best-fit gaussians profiles, except for VCC 190, where two gaussians are fit. (bottom) Normalized residuals from the gaussian fits. The lack of trend demonstrates that all three galaxies are well described by the fits.\label{fig:sample}}
\end{figure*}

\begin{figure}[ht]
\epsscale{1.1}
\plotone{fig-bluecenter.eps}
\caption{Deep CFHT images reveal that VCC 611 has strong star formation concentrated at the galaxy's center. (left) CFHT $i$-band image of the central 4 kpc of VCC 611. (right) $g-i$ color of the same field. The $i$-band image shows a mostly smooth old stellar population, while the $g-i$ color shows that star formation is occurring in the galaxy's center, in several star-forming knots.\label{fig:bluecenter}}
\end{figure}

\subsection{HI Observations}
\label{sec:HI}
\noindent
The HI content of the three dwarf elliptical galaxies in our sample were observed at high spectral resolution (native 0.65 km~s$^{-1}$\ channel width) using the Arecibo Observatory. Observations were performed with the LBW receiver in a series of 5 minute ON/OFF pairs. Results are summarized in Table 2. The ALFALFA data cubes indicate that there are no sources within $10^\prime$ which could be contaminating the sources by being detected in Arecibo's sidelobes above the 5\% level.

The \mbox{H\textsc{i}}\ spectra of the three galaxies are shown in Figure~\ref{fig:sample} (third row). VCC 611 and VCC 1533 (center and right) are in good agreement with a gaussian profile: the normalized residuals (bottom center and right) show low scatter and non-significant trends. In addition, we fit 3rd order gauss-hermite polynomials, to both spectra to look for asymmetric components. For VCC 611, we find no significant asymmetries, while VCC 1533's \mbox{H\textsc{i}}\ profile is asymmetric at a $3\sigma$ level. The velocity widths of both galaxies are very narrow: $W_{50} = 19$ and $28$ km~s$^{-1}$, respectively). Fit parameters are presented in Table 3.

\begin{deluxetable}{lccccc}
\tablecolumns{5}
\tablewidth{0pt}
\tabletypesize{\scriptsize}
\tablecaption{Sample HI Properties}
\tablehead{
  \colhead{Galaxy} & \colhead{$S_\text{HI}$} & \colhead{$\log M_\text{HI}$} & \colhead{$V_{sys}$}       & \colhead{$W_{50}$}\\
                   & Jy km~s$^{-1}$                 & $\log M_\odot$               & km~s$^{-1}$                      & km~s$^{-1}$\\
                   & (1)                     & (2)                          & (3)                       & (4)}
\startdata
VCC 190 A          & $0.18 \pm 0.01$         & 7.1                          & $2345.4 \pm 0.2$          & $14.9 \pm 0.6$\\
VCC 190 B          & $0.29 \pm 0.02$         & 7.3                          & $2371$ \ \ $\pm$ $2$ \ \  & $46 \pm2$\\
VCC 611            & $0.12 \pm 0.01$         & 6.9                          & $1304.5 \pm 0.6$          & $19 \pm 1$\\
VCC 1533           & $0.45 \pm 0.01$         & 7.5                          & \ $648$ \ \ $\pm$ $1$ \ \ & \ $27.7 \pm 0.6$
\enddata
\tablecomments{\label{tab:spectra}Results of single pixel \mbox{H\textsc{i}}\ spectral observations. VCC 190 is split into a relatively blueshifted (A) and redshifted (B) peak. Column 1: integrated flux density; Column 2: \mbox{H\textsc{i}}\ mass, assuming a distance of 16.7 Mpc; Column 3: heliocentric optical velocity; Column 4: Full-width half maximum of gaussian fit. For VCC 190, the fit is two simultaneous gaussian fits, one to the narrower, low velocity piece, and to the wider, higher velocity tail.}
\end{deluxetable}

The \mbox{H\textsc{i}}\ profile of VCC 190 (Figure~\ref{fig:sample}; third row left) is neither gaussian nor does it have a typical symmetric two-horn profile. Attempting to fit a single, asymmetric profile to the galaxy produces a rather poor fit overall ($\chi^2_\nu = 3.0$). Such asymmetries in the global \mbox{H\textsc{i}}\ profile are typical in galaxies for which ongoing ram-pressure stripping is observed (\citealt{KoopmannKenney2004}; \citealt{OosterloovanGorkom2005}; \citealt{Haynes2007}; \citealt{Chung2007}), though stripping is not the only possible explanation.

Instead, guided by our VLA observations (see \S\ref{sec:vla}), we fit two gaussians, one to the lower redshift peak, and one to the higher redshift peak. The combined model fits the data well ($\chi^2_\nu=1.5$), with no trend in the residuals (bottom left). The lower redshift peak has a very narrow $W_{50} = 15$ km~s$^{-1}$, while the higher redshift peak has $W_{50} = 46$ km~s$^{-1}$.

\subsection{VLA Observations of VCC 190}
\label{sec:vla}
\noindent
We observed VCC 190 using the VLA in the D and C configurations for 2 hours and 4 hours respectively. The cubes were produced in CASA using multiscale clean, with a Briggs robustness weighting of $1.0$. Continuum subtraction was performed in the image plane with the \textsc{imcontsub} task using the line-free channels. This yielded an rms of $1.0$ mJy beam$^{-1}$\ in a $37^{\prime\prime}\times 31^{\prime\prime}$ beam, with  $7$ km~s$^{-1}$\ wide channels. The moment 0 maps were produced by first smoothing the data cubes to half their original spatial resolution and calculating a mask at 3 $\sigma$ (3.0 mJy beam$^{-1}$). This mask was then applied to the original data cube.

\begin{figure*}[!ht]
\begin{center}
\epsscale{1.0}
\plotone{fig-VCC190-VLA.eps}
\end{center}
\caption{VLA \mbox{H\textsc{i}}\ intensity maps of VCC 190 overlaid on a KPNO $r$-band image. There are two separate reservoirs of gas in VCC 190, an undisturbed component corresponding roughly to the optical center of the galaxy, and a wide ($W_{50} = 50$ km~s$^{-1}$) component corresponding to the tail. Contours begin at $3\sigma$ (0.03 Jy km~s$^{-1}$\ beam$^{-1} = 0.2\  M_\odot$ pc$^{-2}$) and increase by $3\sigma$ at each additional contour. (left) Intensity map including gas at all velocities (right) Because the galaxy has two distince peaks, we produce two overlaid maps, one corresponding to the blueshifted peak ($v < 2343$ km~s$^{-1}$; blue solid contours) and the other for the redshifted velocity peak ($v > 2343$ km~s$^{-1}$; red dashed contours). The lower velocity peak corresponds to gas coincident with the optical disk of the galaxy {(VCC 190 A)} while the higher velocity peak corresponds to an \mbox{H\textsc{i}}\ tail {(VCC 190 B)}.
\label{fig:vcc190-vla}}
\end{figure*}

Figure~\ref{fig:vcc190-vla} (left) shows a moment 0 image overlaid on a KPNO $r$-band optical image. Contours begin at $3\sigma$ and increase by $3\sigma$ at each additional contour. The gas is not localized directly on the optical, but shows a tail to the southeast. The total flux recovered by the VLA is $0.44\pm0.01$ Jy km s$^{-1}$, which agrees with the Arecibo flux of $0.47 \pm 0.02$ Jy km s$^{-1}$. In Figure~\ref{fig:vcc190-vla} (right), we overlay two sets of contours, corresponding to the velocities of the two peaks observed at Arecibo. The blue contours, corresponding to the narrow, lower velocity peak ($2320-2343$ km~s$^{-1}$) VCC 190 A roughly coincide with the location of the optical galaxy, with an offset of $12^{\prime\prime}=1$ kpc. The red dashed contours correspond to the wider, high velocity peak ($2343-2374$ km~s$^{-1}$) VCC 190 B correspond solely to the tail.

\section{Galaxy Morphology}
\label{sec:morphology}
\noindent
In H12, we argued that this sample is morphologically well-described as dwarf ellipticals, based on optical morphology and color from relatively shallow imaging. All three galaxies in our refined sample were classified as dwarf ellipticals by \citet{Binggeli1985}, are redder than almost all gas-rich late-type dwarfs in the cluster, and no faint substructure was recovered in the galaxies by either \citet{Lisker2006disk} or \citet{Taylor2012} using stacked SDSS imaging. Do the new, significantly deeper, optical and \mbox{H\textsc{i}}\ observations support this assessment?

In the CFHT images, we observe that only VCC 611 appears by eye to be a `typical' dwarf elliptical: it is smooth and clearly elliptically symmetric. VCC 190 and 1533 are a bit peculiar (see Figure~\ref{fig:sample}, first row): VCC 190 is asymmetric and VCC 1533 is boxy in shape. Such peculiar features are, however, not unusual. Massive elliptical galaxies in the field which are observed to have detectable quantities of \mbox{H\textsc{i}}\ often have peculiar optical morphology, appearing blue, distorted, or with faint disk-like features (e.g. \citealt{diSeregoAlighieri2007}; \citealt{Hau2008}; \citealt{Grossi2009}; \citealt{Serra2012}).

It is possible that VCC 611 is a massive elliptical galaxy, but appears to be a dwarf because it is behind the cluster. This can be tested using surface brightness profiles: all dwarf galaxies (early- and late-type) are expected to have exponential profiles, as compared with the de Vaucouleurs profile of more massive ellipticals.  Using $r$- and $i$-band imaging from KPNO and the CFHT, we observe that exponential profiles do fit all three galaxies very well at radii larger than $5^{\prime\prime}$ (see Figure~\ref{fig:sample}, second row). This measure does not, unfortunately, allow us to differentiate between dwarf ellipticals and irregulars.

The bulk motion of stars and gas in dwarf ellipticals is generally not rotational, but pressure-supported. Typical values of $V_{rot} \lesssim \sigma$, where $\sigma$ is the dispersion velocity. For the stellar component, typical values are $0$ km~s$^{-1}$ $<V_{rot}<30$ km~s$^{-1}$, while $20$ km~s$^{-1}$ $< \sigma_*<40$ km~s$^{-1}$\ (e.g. \citealt{vanZee2004}; \citealt{Rys2013}; \citealt{Toloba2014}). This relationship only seems to break down for the most extreme of the so-called fast-rotating and rotationally supported dwarf ellipticals (\citealt{Beasley2009}).

In agreement with stellar observations of other dwarf ellipticals, all three galaxies in our sample have \mbox{H\textsc{i}}\ profiles which show little sign of rotation. All three can be very well fit with a gaussian profile, with widths of $14$ km~s$^{-1}$ $< W_{50} < 28$ km~s$^{-1}$\ (see Figure~\ref{fig:sample}, bottom two rows). We can estimate a sky-projected rotation velocity via:

\begin{equation}
V_{rot}=\frac{\sqrt{W_{50}^2-\sigma_\text{HI}^2}}{2}
\end{equation}

\noindent where $\sigma_\text{HI} = 11$ km~s$^{-1}$\ is our assumed velocity dispersion, and the factor of two accounts for the integrated spectrum containing both the approaching and receding half of the rotation curve. We then obtain approximate \mbox{H\textsc{i}}\ rotational velocities of $4-13$ km~s$^{-1}$, or $V_{rot} \lesssim \sigma_\text{HI}$.

By comparison, the estimated rotational velocities for other late-type dwarfs is much higher. For late-types dwarfs in the Virgo Cluster observed by ALFALFA, the average rotational velocity is $31$ km~s$^{-1}$, with an interquartile range (IQR) of $18$ km~s$^{-1}$ $< V_{rot} < 40$ km~s$^{-1}$, several times $\sigma_\text{HI}$. The FIGGS sample of field irregulars \citep{Begum2008} are typically narrower, with an average $V_{rot}$ of $39$ km~s$^{-1}$ (IQR of $11$ km~s$^{-1}$ $< V_{rot} < 24$ km~s$^{-1}$. While the rotational velocities of the FIGGS sample just overlaps with our sample, the FIGGS galaxies are also typically of lower mass. Finally, we note that the spectra of most late-type dwarfs in ALFALFA and FIGGS also have a two-horned profile or otherwise show clear features of rotational broadening.

\section{Discussion}
\noindent
Thus, our previous assessment that these galaxies are morphologically dwarf ellipticals appears to hold, regardless of whether we consider surface brightness profiles, visual appearance, or velocity widths.
There are, however, a few peculiarities which must be explained, primarily their large \mbox{H\textsc{i}}\ reservoirs in comparison with other dwarf ellipticals. We now explore two hypotheses about the \mbox{H\textsc{i}}\ content of the galaxies. First, we reconsider the hypothesis of H12 that the gas has been recently accreted. Second, we consider whether these galaxies are a part of the irregular or BCD dwarf population, but are between starburst phases, and so only appear optically red and dead.

\subsection{Gas Accretion}
\label{sec:accretion}
\noindent
{Approximately half of giant elliptical galaxies in the field have been observed to bear \mbox{H\textsc{i}}\ (\citealt{Morganti2006}; \citealt{Hau2008}; \citealt{Grossi2009}; \citealt{Oosterloo2010}; \citealt{Serra2012}). In most cases, these authors attributed the presence of gas to accretion---whether of gas-rich satellites, the cooling of ionized gas, or cold-mode accretion from the intergalactic medium (e.g. \citealt{Struve2010}; \citealt{Davis2011}; \citealt{Serra2012}; \citealt{DeRijcke2013}). However, in clusters, ellipticals do not appear to be accreting \citep{Oosterloo2010}. \citet{Morganti2006}, \citet{Oosterloo2010}, and \citet{Serra2012} observed the \mbox{H\textsc{i}}\ in a combined 54 gas-bearing giant ellipticals in the field and the Virgo cluster. These authors found a wide range of \mbox{H\textsc{i}}\ morphologies, from scattered clouds and tails to regularly rotating \mbox{H\textsc{i}}\ disks. They infer recent or ongoing accretion as the origin of the gas when the \mbox{H\textsc{i}}\ is in the form of clouds, tails, and warped and disturbed disks. \citet{Oosterloo2010} also observed that star formation is generally observed in galaxies where accretion is recent or ongoing. When accretion is not recent, star formation is lacking, even when a galaxy is gas-rich.}

{However, the most appropriate population to compare our sample to is other low-mass early-type galaxies, such as NGC 404 and FCC046 (\citealt{delRio2004}; \citealt{DeRijcke2013}). \mbox{H\textsc{i}}\ has been observed in both galaxies, and attributed by the authors to gas accretion in the last Gyr. Like the more massive ellipticals, the gas in NGC 404 and FCC046 is rotating in a disk. The rotational structure of the gas is clear even in an integrated spectrum: both galaxies have a classic two-horned profile, with a velocity widths of 65 km~s$^{-1}$\ \citep{delRio2004} and 67 km~s$^{-1}$\ \citep{DeRijcke2013}.\footnote{We have re-fit the spectrum of FCC046, as the $W_{50} = 34$ km~s$^{-1}$\ \citet{DeRijcke2013} report is from a gaussian, not two-horned, fit to the spectrum.} We note that the true rotational velocity for NGC 404 must be quite large, as its \mbox{H\textsc{i}}\ disk is observed nearly face-on. For FCC046, the misalignment between the angular momentum of the accreted gas and the stellar component of the galaxy is very clear: the gas is in a polar ring. Like more massive ellipticals, accretion coincides with recent star formation for these dwarfs (\citealt{Thilker2010}; \citealt{DeRijcke2013}).}

{Whether comparing with massive or dwarf ellipticals, it is clear that accreted gas is associated with two features: the \mbox{H\textsc{i}}\ morphology is in the form of gas clouds, streams, or warped or disturbed disks, and the presence of star formation. For our sample---where our primary observations are single dish spectra---the direct observable of \mbox{H\textsc{i}}\ in streams or disks would be a large velocity width ($\gtrsim 50$ km~s$^{-1}$) or a two-horned profile as a signature of a rotating disk. We note however that the spectral features are not a perfect analogue to resolved \mbox{H\textsc{i}}\ morphology and are insufficient to conclusively point to recent accretion as the source of the gas. Most notably, we would be unable to discern the existence of a warp in an otherwise smoothly rotating disk. Instead, we can argue that the lack of such features weakens the case for accretion. Neither wide velocity widths nor two-horned profiles are observed for any of the three galaxies. We do, however, observe evidence of recent star formation in VCC 611 and VCC 1533. For VCC 190, where the \mbox{H\textsc{i}}\ is partially resolved, we do observe a gas tail, but we argue that gas removal is a more plausible explanation (see \S\ref{sec:gasstripping}).}

{Finally, we consider the properties of free \mbox{H\textsc{i}}\ clouds in the Virgo cluster. Such clouds would be the source of the accreted \mbox{H\textsc{i}}\ in our sample. Here we run into a signficant problem. If the accretion is ongoing or recent, then a tidal interaction between the clouds and the galaxies would increase the velocity widths of the clouds' \mbox{H\textsc{i}}\ profiles. However, the velocity profile of the \mbox{H\textsc{i}}\ in each of the three galaxies is much narrower than that of any of the clouds in Virgo, which have $W_{50} \gtrsim 50$ km~s$^{-1}$\ (\citealt{Kent2007}; \citealt{Kent2009}). }

\subsection{Between Bursts of Star Formation}
\label{sec:starburst}
\noindent
The high gas fractions in our sample (see Figure~\ref{fig:colors}, right) and their location at the edge of the cluster (\citealt{Conselice2001}; \citealt{Cen2014}; \citealt{Jaffe2016}) suggest that these galaxies are new arrivals to the cluster. However, essentially all dwarf galaxies in the field show signs of recent star formation, to varying degrees (\citealt{Lee2009}; \citealt{Geha2012}). If these galaxies were quenched prior to arriving in the cluster, then approximately 50\% of their gas reservoirs could have been removed, consistent with \mbox{H\textsc{i}}\ observations (\citealt{Hess2013}; \citealt{Odekon2016}) and simulations (\citealt{Bekki2009}; \citealt{Taranu2014}) of galaxy groups.

In groups, dwarfs with morphological features which are somewhere between irregulars and spheroidal dwarfs are observed (\citealt{Mateo1998}; \citealt{SandageHoffman1991}). We observe such features in our sample: VCC 190 and VCC 1533 show deviations from a purely elliptical shape, and VCC 611 has some star-forming features at its center. Called dwarf transitionals, such galaxies have little ongoing star formation, and often have detectable reservoirs of \mbox{H\textsc{i}}. The star formation history of such galaxies is very similar to irregulars and spheroidals until roughly 1 Gyr ago (\citealt{Weisz2011a}; \citealt{Weisz2011b}).
The general interpretation is that dwarf transitionals are either between major episodes of star formation, or have simply permanently stopped forming stars (\citealt{Grebel2003}; \citealt{Skillman2003}).

The typical dwarf transitional has a lower $M_*$ and much lower GF than our sample (\citealt{Weisz2011a}; \citealt{DeLooze2013}). Our sample could be the gas-rich and more massive tail of the dwarf transitional population, holding on to more of their gas while in the group environment by virtue of their higher total mass. Indeed, our most gas-poor galaxy, VCC 611, appears in the dwarf transitional sample of \citet{DeLooze2013}.

\section{The Tail of VCC 190}
\label{sec:gasstripping}
\noindent
Of the three galaxies in our sample, only VCC 190 has clear ongoing gas removal, as indicated by both its unusual HI spectrum and tail. The two processes most likely to produce such a tail are ram pressure stripping and a tidal interaction with a larger galaxy or galaxies. Which is it?

Evidence for ram pressure stripping is fairly weak. VCC 190's projected position is beyond the $3\sigma$ detection of the ROSAT satellite \citep{Bohringer1994}, where the effects of the ICM should be minimal. In addition, massive galaxies at this distance from the cluster center are not \mbox{H\textsc{i}}\ deficient, and rarely show ram pressure stripping tails \citep{Chung2007}. However, VCC 190 is very low mass, and may be susceptible to ram pressure stripping even when it is too weak for the more massive galaxies.

The tail geometry is also not right for ram pressure stripping. In general, tails point opposite the motion of the galaxy, which generally means they point roughly away from the subcluster center (e.g. \citealt{Chung2007}; \citealt{Roediger2008}; \citealt{Kenney2014}). In this case, the tail should point away from either M87 or M49, to the northwest and west, respectively, but VCC 190's tail points southwest. In addition, tails caused by stripping generally point towards the mean redshift of the cluster, as the removed gas is decelerated relative to the ICM, but VCC 190's tail is blueshifted towards higher velocity.

Instead, the tidal interaction hypothesis is stronger. First, we note that the distribution of stars in VCC 190 is not a smooth ellipse, but asymmetric; the top left portion of the galaxy has a higher surface brightness than the bottom right. Ram pressure stripping would only disturb the gas in the galaxy, while a strong tidal encounter, or multiple weaker encounters can disturb the stars as well.

Second, it is clear which galaxies collided with VCC 190. With the exception of a few dwarf galaxies, three galaxies are within 100 kpc of VCC 190 and at a similar redshift, all to the southwest. Figure~\ref{fig:vcc190-environment} shows an optical image with ALFALFA contours overlaid of these galaxies. NGC 4224 and AGC 221988 are interacting, with a tidal bridge visible between them (see Figure~\ref{fig:vcc190-environment}). \citet{Miskolczi2011} found stellar tidal streams coming off of NGC 4224 pointing to the north, for which they could not find an obvious interaction partner; we suggest that AGC 221988 is the cause. An optical spectrum indicates that NGC 4233 is at the same redshift, and so may be interacting with the other galaxies. But, its lack of \mbox{H\textsc{i}}\ means that such an interaction unseen in the image.

The tidal tail of VCC 190 points toward NGC 4224, suggesting an encounter between the two. In addition, NGC 4224 lies at a slightly higher redshift ($v = 2606$ km~s$^{-1}$) than VCC 190 ($v = 2345$ km~s$^{-1}$). As VCC 190 passed by NGC 4224, the removed gas in VCC 190's tail would be perturbed to a higher redshift, as is observed. We performed additional observations at Arecibo between VCC 190 and NGC 4224 (Figure~\ref{fig:vcc190-environment}; red crosses) to look for a tidal bridge between the two galaxies. No gas was detected, with a $3\sigma$ upper limit of $10^{6.3} M_\odot$ (0.10 Jy km~s$^{-1}$), assuming a $30$ km~s$^{-1}$\ wide tail, or approximately 5\% of the \mbox{H\textsc{i}}\ mass of VCC 190.

\begin{figure}[!ht]
\begin{center}
\epsscale{1.15}
\plotone{fig-VCC190-environment.eps}
\end{center}
\caption{The environment of VCC 190. The tidal tail of VCC 190 points towards NGC 4224, suggesting a tidal encounter between the two. NGC 4224 is itself interacting with AGC 221988. Background is a DSS-2 composite optical image, while the overlaid contours are an \mbox{H\textsc{i}}\ column density map; contour levels are identical to Figure \ref{fig:vcc956-environment}. All galaxies with redshifts consistent with the Virgo Cluster are labeled. The red crosses are the locations of additional Arecibo pointings used to detect a bridge between NGC 4224 and VCC 190; no gas was detected at any of the three pointings.
\label{fig:vcc190-environment}}
\end{figure}

Based on the disturbed and asymmetric stellar light distribution in the galaxy, the presence of a narrow and undisturbed ($W_{50} = 14$ km~s$^{-1}$) component of HI centered on the optical galaxy, and finally NGC 4224 as a clear collision partner, this tail is likely to be tidal in nature.

\section{Summary}
\label{sec:conclusions}
\noindent
We revisited sample of dwarf elliptical galaxies in the Virgo Cluster identified by H12. Despite being `red and dead,' all had substantial reservoirs of \mbox{H\textsc{i}}\ as detected in ALFALFA. We found that the two lowest signal-to-noise \mbox{H\textsc{i}}\ detections reported in H12 and \citet{Haynes2011}, VCC 421 and VCC 1649, were spurious. We further eliminated two more galaxies from the sample of H12: VCC 956 appears at the same sky location as a long \mbox{H\textsc{i}}\ tidal tail off of NGC 4388, and VCC 1993 is not a dwarf galaxy. Our primary sample of interest was thus narrowed to three galaxies: VCC 190, VCC 611, and VCC 1533.\\
\\
\textbf{New radio and optical observations.} High resolution (channel width of 0.65 km~s$^{-1}$) Arecibo observations reveal that VCC 611 and 1533 have narrow ($W_{50}<30$ km~s$^{-1}$) velocity widths and gaussian profiles. VCC 190 has two gaussian peaks, one narrow and one wide ($W_{50}=45$ km~s$^{-1}$). VLA observations of VCC 190 show an \mbox{H\textsc{i}}\ tail pointing toward NGC 4224 to the south, and the tail corresponds to the wide velocity feature observed at Arecibo. The ALFALFA data cubes show that NGC 4224 is interacting with one of its neighbors, AGC 221988.

Our KPNO observations and CFHT archival data from the NGVS show that all three galaxies have exponential profiles and lack widespread star-forming features. They do have some unusual features, however: the surface brightness of VCC 190 is asymmetric, VCC 611 has a star-forming feature at its center, and VCC 1533 is boxy in shape.\\
\\
\textbf{Elliptical morphology without significant removal of gas} is observed for all three galaxies, even though gas removal in clusters should be very rapid compared with morphological change. This is supported both by their optical (exponential profiles and a lack of widespread star-forming features) and \mbox{H\textsc{i}}\ (narrow, undisturbed velocity profiles) features. Together, these features suggest that the galaxies are relatively new arrivals in the cluster which have not {undergone significant gas stripping. We observe ongoing gas removal in VCC 190 (see below), but the current tidal interaction is too recent to be responsible for its optical properties.}

These galaxies are similar to dwarf transitionals---galaxies with optical morphologies between irregulars and spheroidals with little sign of star formation. All three galaxies show some deviation from a smooth elliptical shape; VCC 190 is asymmetrical, VCC 611 has ongoing central star formation, and VCC 1533 is box-like in shape. Transition-type dwarfs may be between bursts of star formation; our sample additionally may have been weakly stripped ($<50$\% gas removal) while still in a group environment. Our sample is more gas rich and has a higher $M_*$ than is typical for dwarf transitionals (\citealt{Weisz2011a}; \citealt{DeLooze2013}), and so we could be observing the most extreme galaxies in the transition population.\\
\\
\textbf{Ambiguous evidence for gas accretion.} {In elliptical galaxies with accreted gas, recent or ongoing star formation is generally observed, and the \mbox{H\textsc{i}}\ is in the form of clouds, streams, or a perturbed rotating disk. For two galaxies in our sample, we do observe star formation: the SDSS spectrum of VCC 611 shows strong centrally-located star formation, and the overall color of VCC 1533 is at the edge of what is expected for star-forming dwarfs (NUV$-r=3$). With single-dish spectra, we can only imperfectly probe the \mbox{H\textsc{i}}\ morphology, but an \mbox{H\textsc{i}}\ disk will have a clear two-horned profile, and both disks and streams have wide velocity widths even in dwarfs ($W_{50}\gtrsim50$ km~s$^{-1}$). The \mbox{H\textsc{i}}\ lines of VCC 611 and VCC 1533 galaxies are both narrow ($W_{50}<30$ km~s$^{-1}$) and lack evidence of rotation as both are well-fit by a gaussian profile. VCC 190 is not star-forming, and the \mbox{H\textsc{i}}\ at its optical position is similarly non-rotating. A tail is evident in \mbox{H\textsc{i}}\ imaging of VCC 190, but is more consistent with gas removal than accretion.}\\
\\
\textbf{Evidence of tidal gas removal in VCC 190.} An observed \mbox{H\textsc{i}}\ tail in VCC 190 points towards NGC 4224, while the gas coincident with the optical galaxy is practically undisturbed (fit well by a gaussian with $W_{50} = 15$ km~s$^{-1}$). The tail is redshifted relative to the \mbox{H\textsc{i}}\ in the optical galaxy, as would be expected from an encounter with NGC 4224, which is at a higher redshift than VCC 190. These all suggest that the tail is a tidal feature from an encounter approximately 1 Gy ago.
\\
\section*{Acknowledgements}
\noindent
We are extremely grateful for the observations performed by the faculty and students of the Undergraduate ALFALFA Team (UAT), without which this work would not be possible.  They performed the observations at Arecibo to confirm each galaxy's \mbox{H\textsc{i}}, and performed the optical observations at KPNO of VCC 190 and VCC 611. The UAT is supported by NSF grant AST-1211005.\\
\\
ALFALFA has been supported by NSF grant AST-1107390, and grants from the Brinson Foundation.\\
\\
This work is based in part on observations made with the Karl G. Jansky Very Large Array, a facility of the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\\
\\
This work is based in part on observations made with the Arecibo Observatory. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. M\'{e}ndez-Universidad Metropolitana, and the Universities Space Research Association.\\
\\
This work is based in part on observations made with the WIYN 0.9m telescope operated by WIYN
Inc. on behalf of a consortium of nine partner Universities and Organizations.

redpajama_set_name: RedPajamaArXiv


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