text:
Accepting a JSON request body
=============================

A common need when building a restful API is the ability to accept a JSON
encoded entity from the request body.

An example for such an API could be a blog post creation.

Example API
-----------

In this example we will create an API for creating a blog post. The following
is a spec of how we want it to work.

Request
~~~~~~~

In the request we send the data for the blog post as a JSON object. We also
indicate that using the ``Content-Type`` header:

.. code-block:: text

    POST /blog/posts
    Accept: application/json
    Content-Type: application/json
    Content-Length: 57

    {"title":"Hello World!","body":"This is my first post!"}

Response
~~~~~~~~

The server responds with a 201 status code, telling us that the post was
created. It tells us the ``Content-Type`` of the response, which is also
JSON:

.. code-block:: text

    HTTP/1.1 201 Created
    Content-Type: application/json
    Content-Length: 65
    Connection: close

    {"id":"1","title":"Hello World!","body":"This is my first post!"}

Parsing the request body
------------------------

The request body should only be parsed as JSON if the ``Content-Type`` header
begins with ``application/json``. Since we want to do this for every request,
the easiest solution is to use an application before middleware.

We simply use ``json_decode`` to parse the content of the request and then
replace the request data on the ``$request`` object::

    use Symfony\Component\HttpFoundation\Request;
    use Symfony\Component\HttpFoundation\ParameterBag;

    $app->before(function (Request $request) {
        if (0 === strpos($request->headers->get('Content-Type'), 'application/json')) {
            $data = json_decode($request->getContent(), true);
            $request->request->replace(is_array($data) ? $data : array());
        }
    });

Controller implementation
-------------------------

Our controller will create a new blog post from the data provided and will
return the post object, including its ``id``, as JSON::

    use Symfony\Component\HttpFoundation\Request;
    use Symfony\Component\HttpFoundation\Response;

    $app->post('/blog/posts', function (Request $request) use ($app) {
        $post = array(
            'title' => $request->request->get('title'),
            'body'  => $request->request->get('body'),
        );

        $post['id'] = createPost($post);

        return $app->json($post, 201);
    });

Manual testing
--------------

In order to manually test our API, we can use the ``curl`` command line
utility, which allows sending HTTP requests:

.. code-block:: bash

    $ curl http://blog.lo/blog/posts -d '{"title":"Hello World!","body":"This is my first post!"}' -H 'Content-Type: application/json'
    {"id":"1","title":"Hello World!","body":"This is my first post!"}


This costume is actually the skirt from my Serenity costume, taken in about 6+ inches and hiked up. I styled the wig in about an hour, and someone found me a fork at the convention. It's just a hoot to wear this and laugh with people when they realize who I am.


text:
package com.visionarysoftwaresolutions.smacker.api.events;

import com.visionarysoftwaresolutions.eventr.Event;
import com.visionarysoftwaresolutions.smacker.api.User;
import com.visionarysoftwaresolutions.smacker.api.meals.Meal;

public interface MealNotification extends Event {
    User getUser();
    Meal getMeal();
}

redpajama_set_name: RedPajamaGithub


Bas, A.A., Christiansen, F., Öztürk, B., Öztürk, A.A., Erdog˘an, M.A. and Watson, L.J. (2017) Marine vessels alter the behaviour of bottlenose dolphins Tursiops truncatus in the Istanbul Strait, Turkey. Endangered Species Research, 34 . pp. 1-14.
The non-lethal impacts of marine vessels on cetaceans are now a globally recognised threat. This study is the first to investigate the effect of marine traffic on the behaviour of bottlenose dolphins Tursiops truncatus in the Istanbul Strait, Turkey. The Istanbul Strait (also known as the Bosphorus) is one of the busiest international waterways in the world and is exposed to dense marine traffic. The effect of marine traffic, location and season on the behavioural transitions was investigated through general log-linear analysis. Further, the changes on the behavioural budget and bout duration were assessed using Markov chains. Results showed that marine vessels were the main driving force for the behavioural transitions. These changes in transitions between behaviours led to significant changes in behavioural budget and bout durations (average time in each behavioural state). Surface-feeding, resting and socialising behaviour significantly de creased in the control budget, while diving showed an increase in the presence of vessels. Moreover, dolphins spent less time surface-feeding, resting, socialising and diving once disrupted. Furthermore, the current level of vessel-dolphin interaction (51%) in the Istanbul Strait was sufficiently high to alter the dolphins' cumulative behavioural budget significantly. Finally, speed and distance of vessels played a considerable role in the directional responses of dolphins. These results raise concerns on the potential biological consequences of the observed behavioural changes, considering that the population is already classified 'at risk' and is still lacking species-specific conservation plans. The results of the study must be considered immediately to create protected zones in order to mitigate the vessel-dolphin interactions.


text:
Interview: Leon of Athens (Coffee House Sessions)
February 19, 2018 February 9, 2018 mgr511
Image Credits: Press Pack
London-based Greek indie-pop star Leon of Athens will be releasing his forthcoming album Xenos, produced by David Kosten (Bat For Lashes, Marina & The Diamonds) on 9th February. Channelling a similar widescreen pop sensibility as Bastille, James Bay and M83 alongside the flamboyant beauty of Sufjan Stevens, Bright Eyes, Perfume Genius and Tame Impala, the album Xenos is a beautiful, thoughtful piece of work. It showcases just why he has become a huge live draw in Greece – where he plays to audiences in their thousands – his ever-growing fan base across Europe and his rising profile in the USA where he has just been confirmed to appear at Okeechobee Festival and South By South West in March. From the uplifting indie-pop of the singles 'Aeroplane' and 'Fire Inside You', to the dark creeping electronics of the title track and 'Xenos', Leon Of Athens proves himself an intriguing and exciting force.
This interview is part of a series of syndicated interviews with the artists that will take part in the Coffee House Sessions at The Courtyard, University of York, during this term.
You'd describe your music as…
Indie-pop
You're currently listening to…
Tame Impala, Kimbra, Kendrick Lamar, Sufjan Stevens
When you're not making music you're…
I watch movies.
You'd like to duet with…
Florence and FKA Twigs
Who's your guilty pleasure?
No shame, no guilt, Bee Gees and ABBA.
Dead or alive, who would you most like to grab a coffee with?
David Bowie and Bob Marley
You're an artist because…
It's the most magical way to connect with yourself and other people.
Vinyl, CD or Streaming…
Vinyl, no doubt!
Your party trick is…
-blank-
Your hometown is… and we should visit because…
Originally, I'm from Athens but now I live in London. You should definitely visit Athens, it's an amazing city, sleepless at night and sunny in the morning. Not to mention the history and vibe.
Tinder or taken?
Taken is a great app, highly recommend it:)
Snapchat, insta or twitter?
The best boxset is…
The Godfather and The Beatles boxset.
Coffee House Tour … what are you most excited about?
Every single show. I just can't wait!
Leon of Athens' Most Frequently Used Emojis
Follow Leon of Athens
Enjoy live music from Leon of Athens in The Courtyard, Derwent College at 7 pm on Thursday 22nd February.
mgr511
Arts & Culture, Features, Music Coffee House Sessions, Interview, Leon of Athens
← Need for YUSU reform is clear
The Strike Debate →

redpajama_set_name: RedPajamaCommonCrawl


Wild species with valuable genetic heritage was used long time ago in interspecific crosses to improve cultivated plants adaptation to environmental constraints. The objective of this study is to transfer the salinity tolerance of Hordeum marinum, a wild barley species, to three durum wheat varieties (Karim, Razzek and Nasr) by intergeneric crosses. In order to skip the incompatibility between these species, in vitro immature embryo rescue was performed using B5 medium (Gamborg et al., 1968). The results showed that the genotype has an important effect on the success of the crosses and the rate of regenerated plants. We have found that 34.21% of the embryos derived from hybridization Razzek x Hordeum marinum has regenerated haploid plantlets, 5.88% for Karim x Hordeum marinum cross, and 2.78% for Nasr x Hordeum marinum.
The obtained chromosomal stock of the hybrid haploid plants was doubled by colchicine treatment concentrated at 0.05%. The rate of doubled haploid plants were reduced after colchicine treatment to 26.32% for Razzek x Hordeum marinum cross, 0% for Karim crossed with Hordeum marinum and remained unchanged for Nasr x Hordeum marinum.
The doubled haploids obtained are subjected to salt stress (6-12 g/l) in order to evaluate their tolerance to salinity.


text:
Occasional Train Blogging: Double-Deck Trains part deux | 35 comments (35 topical, editorial, 0 hidden)
Re: California Zephyr (none / 1)
I'm taking the train home for Christmas. The train is $70 roundtrip (that's including a business class upgrade, it's $42 coach) whereas the cheapest flight I found was for $182.
It is slower, of course, but I can also get a lot done on a train. And the station is about a block from my family's home whereas the airport, with holiday congestion, is about a 45 min drive.
Those who can make you believe absurdities can make you commit atrocities. -Voltaire
by p------- on Wed Nov 29th, 2006 at 10:36:26 AM EST
I just enjoy being on a train or bus - I still have some of that schoolboyish enthusiasm for it. I've never got used to planes or cars - you can't relax. I can even daydream on a train, inspired by what I see out of the windows.
Of course a car drive is also sometimes a good way to solve an impossible conceptual problem that's been going around in your mind. Focusing on driving seems to bring a different kind of thinking into play - ie not thinking consciously.
But I still couldn't tell you exact model of Fiat I have apart from the name, nor the licence number. I just don't care.
You can't be me, I'm taken
by Sven Triloqvist on Wed Nov 29th, 2006 at 10:59:35 AM EST
I know your question wasn't directed at me, but I just bought the tickets last night and am still in shock about the price difference. I think it means the trains are desperate for business. Kinda sad.
Maybe they also compete with Greyhound?
by DoDo on Wed Nov 29th, 2006 at 11:39:56 AM EST
How long is the trip?
by Colman (colman at eurotrib.com) on Wed Nov 29th, 2006 at 11:23:50 AM EST
Check AMTRAK's schedule. Apparently, scheduled for 18 hours 40 minutes over 1038 miles.
Sorry, I thought you are asking asdf, about the Denver-Chicago trip...
by DoDo on Wed Nov 29th, 2006 at 02:34:47 PM EST
Re: California Zephyr (4.00 / 3)
4.5 hours, compared to a 45 min flight! LOL. But the difference is really diminished when you factor in the commute to and from the airport, the fact that you are supposed to get to the airport 2 hours early and of course, the holiday crowds that exacerbate everthing. Door to door it is about 4 hours to take the plane home, and a little over 5 hours to take the train.
Exactly. Flight times are grossly misleading.
Those whom the Gods wish to destroy They first make mad. -- Euripides
by Migeru (migeru at eurotrib dot com) on Wed Nov 29th, 2006 at 11:56:49 AM EST
And when you allow for the much more useful time expenditure on a train you're way ahead ...
by Colman (colman at eurotrib.com) on Wed Nov 29th, 2006 at 12:04:20 PM EST
When I lived in Boston it was cheaper to fly to NYC than to take the train, even the non-Accela train. Tickets were about 200 for the non-Accela train round trip. What I usually did was drive half way to New Haven, CT (10 bucks for gas) and take the commuter rail into town (20 bucks one way) for a total cost of 60 bucks.
In other news, we should have a bullet train running from Portland, ME to Washington DC. It is ridiculous to not have better rail service on the east coast. It won't happen as long as we keep on subsidizing our failing airlines.
you are the media you consume.
by MillMan (millguy at gmail) on Wed Nov 29th, 2006 at 01:24:29 PM EST
Why is it that subsidizing rail is evil but subsidizing airlines is necessary?
by Migeru (migeru at eurotrib dot com) on Wed Nov 29th, 2006 at 01:26:16 PM EST
The automobile completely destroyed the passenger rail industry in the US. Had the rail industry survived in any serviceable form we would likely be subsidizing them to the same degree as the airlines today, as the rail industry would have had lobbyists with long, deep ties to various politicians of the sort that the airline, auto, and telecom industries have.
Ironically, US rail's fall from favour was partly due to heir earlier strong meddling in politics, they didn't got the subsidies in the first half of the 20th century because that was then how politicians demonstrated that they aren't corrupt.
Occasional Train Blogging: Double-Deck Trains part deux | 35 comments (35 topical, 0 editorial, 0 hidden)


text:
Keywords:desertification
The term DESERTIFICATION was coined in 1949 by A. Aubreville, a French scientist working in West Africa. Aubreville introduced this umbrella term to describe several ecological processes in tropical Africa, in particular the progressive transformation of tropical forests in savanna and drier ecosystems. In advancing this term, Aubreville was attempting to describe the way in which the Sahara Desert was expanding to engulf desert-marginal savanna grasslands. The term was further popularized in the 1970s because of the prolonged Sahelian drought. Since then, desertification has aroused intense debate in the scholarly community about the extent, definition, causes, and how to control this phenomenon, which has led to multiple definitions. In 1983, Michael Glantz and Nicolai Orlovsky reported encountering more than one hundred definitions of desertification in ...
Design (and Ecodesign)
Robbins, P. (2007). Desertification. In Encyclopedia of environment and society (Vol. 1, pp. 450-451). SAGE Publications, Inc., https://dx.doi.org/10.4135/9781412953924.n293
Robbins, Paul. "Desertification." In Encyclopedia of Environment and Society, edited by Robbins, Paul, 450-51. Thousand Oaks, CA: SAGE Publications, Inc., 2007. https://dx.doi.org/10.4135/9781412953924.n293.
Robbins, P. 2007. Desertification. In: Paul Robbins Editor, 2007. Encyclopedia of Environment and Society, Thousand Oaks, CA: SAGE Publications, Inc. pp. 450-451 Available at: <https://dx.doi.org/10.4135/9781412953924.n293> [Accessed 20 Jan 2022].
Robbins, Paul. "Desertification." Encyclopedia of Environment and Society. Edited by Vol. 1. Thousand Oaks: SAGE Publications, Inc., 2007, pp. 450-51. SAGE Knowledge. 20 Jan 2022, doi: https://dx.doi.org/10.4135/9781412953924.n293.
https://sk.sagepub.com/Reference/environment/n293.xml


Jenna Coleman has confessed she was once asked to wear a bikini for an audition.
The 32-year-old actress first rose to prominence in British soap Emmerdale before landing a role in cult BBC show Doctor Who, as the Time Lord's assistant Clara Oswald. Since then, she has achieved leading lady status in critically acclaimed drama Victoria, in which she plays the titular role of British monarch Queen Victoria.
However, in an interview with The Guardian, which discussed whether she had experienced overt sexual harassment in the industry, Jenna denied she had, but recalled an inappropriate request that occurred when she went to try her luck in Hollywood over 10 years ago.
"I was asked to turn up to an audition in a bikini and just said no," she told the newspaper. "You know, there's been silly things like that," she shared when asked about sexism in the entertainment industry.
Jenna is in the middle of filming the third series of the hit ITV drama, scripted by Daisy Goodwin. But when asked about her awareness of equal pay in her roles she said it's "really hard" because actors rarely share information about salaries.
"It's really hard for me because obviously the last couple of projects I've been doing, I've been in a comfortable position where I've been able to be strong… But the thing is, nobody talks," she sighed.


text:
GATEWAY ANNOUNCES 2019 NASCAR GANDER OUTDOORS TRUCK SERIES DATE
June 9, 2018, St. Louis Region – Gateway Motorsports Park in Madison, Illinois, today announced its 2019 NASCAR Truck Series date: Saturday, June 22, 2019. Additionally, NASCAR has changed the name of the series to the NASCAR Gander Outdoors Series.
"We are pleased once again to be a part of the NASCAR's Gander Outdoors Truck Series," said Chris Blair, Gateway Motorsports Park's Executive Vice President and General Manager. "Five years ago, when we signed our first agreement with NASCAR, a lot of people thought we would be a one-year experiment. This proves we are a longstanding fixture and important part of NASCAR's racing program. Events like the NASCAR Gander Outdoors Truck Series, INDYCAR, NHRA and our ARCA event are very important in developing the future of motorsports in St. Louis. If we continue to demonstrate how much the fans love the racing at Gateway Motorsports Park, other opportunities may come our way for bigger and better events."
Gateway Motorsports Park's annual NASCAR weekend will begin on Friday, June 22 with the Papa Nicholas 150 for the ARCA Racing Series presented by Menards. The annual Villa Lighting delivers the Eaton 200 presented by CK Power NASCAR Camping World Truck Series race follows on Saturday, June 23 at 7:30 p.m. CDT. To purchase tickets or obtain additional information, please call Gateway Motorsports Park at (618) 215-8888 or visit www.wwtraceway.com. Follow GMP on Facebook, Twitter, Snapchat and Instagram.
About Gateway Motorsports Park
Gateway Motorsports Park is the home of INDYCAR, NASCAR and NHRA racing in the St. Louis region. Located just five minutes from downtown St. Louis and covering more than 340 acres, Gateway Motorsports Park is the largest outdoor entertainment facility in the area. Gateway Motorsports Park's facilities include a 1/4-mile drag strip, 1.25-mile superspeedway, 1.6-mile road course, a state-of-the-art karting facility and a 14-acre, multi-purpose dirt off-road venue. Gateway Motorsports Park was the recipient of the 2017 Outstanding Facility of the Year Award from the Race Track Business Conference and the 2017 Spirit of St. Louis Award from St. Louis Attractions Association.
gateway2018-06-13T15:25:21+00:00June 13th, 2018|Blog, News|


text:
Realcuba's Blog
against mediaterror and for freedom of cuban 5
Posts Tagged 'dolores huerta'
Angela Davis, Danny Glover, Dolores Huerta, Ignacio Ramonet, Mighty Gabby and many others to join "5 Days for the Cuban 5 in Washington DC"
( Photo: Bill Hackwell/Rally in front of the White House April 2012 )
From May 30 to June 5th 2013, a number of well-known intellectuals, authors, artists, labor, religious figures, attorneys, and supporters of the Cuban 5 will gather in Washington DC to advocate for a dialogue between the United States and Cuba, to raise awareness about the case of the Cuban 5 and to demand a humanitarian solution that will allow the return of these men to their homeland.
This week of activities is a result of a call made in November 2012 during the VIII Colloquium in Holguin for the Freedom of the Cuban 5 and against terrorism.
The Second "5 Days for the Cuban 5 in Washington DC" is being organized by the International Committee for the Freedom of the Cuban 5, sponsored by the Institute for Policy Studies (IPS) and endorsed by more than 50 organizations and individuals.
MIGHTY GABBY FROM BARBADOS CONFIRMED!
Mighty Gabby, Cultural Ambassador from the Island of Barbados will come to Washington to participate in the week of events. He won the calypso crown in Barbados at age 19 in 1968 and went on to win the Calypso king title again in 1969, 1976, 1985, 1999, 2000 and again in 2010. He has written over 700 songs and was awarded Folk Singer Of The Year in 1977, 1978, 1979. Below is a song he wrote about the Cuban 5 called FREE THEM (See http://youtu.be/JmS4kHC_OlY, )
AGENDA FROM MAY 30 TO JUNE 5
THURSDAY MAY 30
9:00am: Press Conference. Wayne Smith, Dolores Huerta, Ignacio Ramonet, Yeidckol Polevnsky, Fernando Morais, lawyers and other guests. Place: National Press Club, 529 14th Street NW, 13th Floor, Bloomberg Room, Washington, DC.
9:30am-5:00pm: Booth with information about the Cuban 5 at the Latin American Studies Association (LASA) conference. Place: Washington Marriott Wardman Park, 2660 Woodley Road NW, Washington, DC.
5:00pm: Important orientation meeting: Place: Howard University Hospital 2041 Georgia Ave NW, Ambulatory Care Center/Towers Building, Auditorium, First Floor, Washington, DC 20060, (There is parking in back of the hospital and also an entrance off of 5th street, between Elm and V streets.) The orientation will be followed by the 7pm meeting at the same location.
7:00pm: Role of Cuba in Africa and the Cuban 5 in Angola. Excerpt from the revealing and award winning documentary Cuba: An African Odyssey and an interactive panel discussion with representative of the Cuban Interest Section in Washington, representatives from the Embassy of Namibia, Eugene Puryear from the ANSWER Coalition, Mary-Alice Waters from Pathfinder Press and Glen Ford, co-founder and Executive Editor of Black Agenda Report." Place: Howard University Hospital 2041 Georgia Ave NW, Ambulatory Care Center/Towers Building, Auditorium, First Floor, Washington, DC 20060, (There is parking in back of the hospital and also an entrance off of 5th street, between Elm and V streets.)
FRIDAY MAY 31
9:30am – 5:00pm: Booth with information about the Cuban 5 at the Latin American Studies Association (LASA) conference. Place: Washington Marriott Wardman Park, 2660 Woodley Road NW, Washington, DC.
10:00am – 5:00pm: Washington area outreach. Pick up literature and assignments for distributions at busy Metro stops and other public places. Place: Institute for Policy Studies, 1112 16th St. NW, Suite 600, Washington, DC.
3:00pm: Meeting of Cuban nationals and Cuban Americans who live in the U.S. to plan new strategies among other issues, about the U.S. campaign to free the Cuban 5 (by invitation only)
7:00pm: Reception (by invitation only)
SATURDAY JUNE 1ST
1:00pm: Rally in front of the White House, across the street from Lafayette Park. Activists are coming from Quebec and many U.S. cities, including a large delegation of Cuban Americans from Miami. The June 1st Organizing Committee based in New York City is organizing buses to join the DC rally. Tickets are $5 roundtrip with lunch included. Buses will be leaving from the Bronx (Hostos Community College), El Barrio/East Harlem (Julia de Burgos Cultural Center), Washington Heights (Port Authority Bus Terminal/179 Street & Broadway) and from D.C. 37-Local 372 and the Martin Luther King, Jr. Labor Center/1199-SEIU, Manhattan. To reserve your seat from NYC, call 347-201-3728. Rally Program will include speakers representing diverse voices from the struggle to free the Cuban 5 from the U.S. and abroad, plus entertainment.
6:00pm: Ecumenical-Cultural Event. Special Guests: Angela Davis, Nacyra Gómez Cruz, Presbyterian Reformed Church in Cuba, Secretary of International Relations of the Christian Conference for Peace for Latin America and the Caribbean, Maria León (from the Venezuela National Assembly) Yeidckol Polevensky (former Vice President of the Mexican Senate). Poetry by Andy de la Tour, English actor and screenwriter. Music by Mighty Gabby, a Cultural Ambassador for the island of Barbados who sings Calypso and the DC Labor Chorus. Place: Saint Stephen Church, 1525 Newton St. Washington DC.
SUNDAY JUNE 2
11:00am: Community Event. Gathering at 11am in downtown Takoma Park (between Carol Ave and Laurel) to walk back to Place: Casa Rutilio, 102 Park Ave, for a community event at 1:00pm. This event is organized by the Takoma Park Free the Cuban 5 Committee and endorsed by the DC Metro Coalition to Free the Five and the International Committee for the Freedom of the Cuban 5. Music by Ismael "Bandolero" Duran and Patricio Zamorano.
2:30pm: Hip Hop Cultural Event with Head Roc and Mighty Gabby. Head Roc, for nearly 20 years has been regarded as the best that DC Hip-Hop has to offer. He has come to embody the passions, hopes and dreams of a wonderfully talented DC Black music scene. Opening remarks by Rev. Graylan Hagler, Senior Minister of Plymouth Congregational United Church of Christ and National President of Ministers for Racial, Social and Economic Justice. Place: Plymouth Congregational United Church of Christ, 5301 North Capitol Street, NE Washington, D.C
MONDAY JUNE 3
9:00am: Lobby activities. Members of Parliaments from other countries who have confirmed their participation: Yeidckol Polevensky (former Vice President of the Mexican Senate), Maria León (Venezuela) a Member of Parliament from El Salvador, Gianni Vattimo, (Italy), Hugo Gutierrez and Alejandro Navarro (Chile) and others to be confirmed.
11:00am: Meeting with attorneys and jurists from the U.S. and abroad. Convened by Martin Garbus, attorney of the legal team of the Cuban 5 with the presence of lawyers from the U.S. and abroad including former U.S. Attorney General Ramsey Clark, Peter Schey from the Center for Human Rights and Constitutional Law, Jose Pertierra, Attorney representing Venezuela in the case of the extradition of Luis Posada Carriles to Venezuela, Rafael Anglada from Puerto Rico, Fabio Martelli and Tecla Faranda from Italy, Beinusz Szmukler from Argentina, Graciela Rosemblum President of the Argentinean Human Rights League, and many others. Sponsored by the National Lawyers Guild. Place: Georgetown Legal Center, 600 New Jersey Avenue, N.W., Washington, D.C.
6:00pm: Meeting of elected union leaders and rank and file members from the U.S. and abroad. Welcome from Dena Briscoe, President, American Postal Workers Union Local 140. Special guests: Dennis Lemelin, National President, Canadian Union of Postal Workers, Santos Crespo, President, Local 372 New York City Board of Education and more. Find out why unions in Canada, Ireland and Britain support freedom for the Cuban 5 and how the movement is building in the U.S. Place: Postal Workers Union Hall, 6139 Chillum Place NE, Washington, D.C. 20011.
7:00pm: Opening of an art exhibit of new paintings by Antonio Guerrero followed by a panel of intellectuals. This exhibit is comprised of 15 new paintings by Antonio Guerrero reflecting the 17 months the Cuban 5 spent in the "Hole" and will be introduced by by Gilbert Brownstone, artist, curator, collector and philanthropist. The panel will discuss Cuba in contemporary times and will include Ignacio Ramonet, Spanish writer and former editor-in-chief of Le Monde Diplomatique, Jane Franklin, author, historian and expert on Cuba-U.S. relations, Miguel Barnet, writer and current President of the National Union of Artists and Writers of Cuba (UNEAC) and Salim Lamrani, French professor, author and researcher. Place: Busboys and Poets, 2021 14th Street, NW.
9:00am: Lobby activities continue
11:00am: Reception at Capitol Hill hosted by a U.S. Congressman to welcome the Parliamentarians from other countries (Place TBA)
6:00pm: Panel discussion and book presentations by Brazilian and Canadian authors about democracy in Cuba and the case of the Cuban 5. Panelists: Fernando Morais, Brazilian journalist and author of: The Last Soldiers of the Cold War, Stephen Kimber, Canadian journalist, professor and and author of What Lies Across the Water, and Arnold August, writer, and lecturer from Montreal, author of Cuba and Its Neighbours: Democracy in Motion. Celebration of Gerardo Hernandez's birthday. Place: Busboys and Poets, 2021 14th Street, NW
WEDNESDAY JUNE 5
9:00am: Last day of Lobby Activities
5pm: The 5th for the Cuban 5 closing event: An art exhibit of a motorcycle journey throughout Latin America by graduates from the Latin American School of Medicine in Cuba that promoted awareness about the Cuban Five. Video conference with family members of the Cuban Five from Havana and guests in Washington D.C. Special guest: Danny Glover and Ambassadors from ALBA countries. Plenary Session with organizers from the U.S. and abroad discussing work and future actions is support of the struggle to free the Cuban 5. Music by Mighty Gabby. Place: Embassy of the Bolivarian Republic of Venezuela- Bolivarian Hall, 2443 Massachusetts Avenue, NW, Washington, DC.
Send your endorsement to: apoyojornada@gmail.com
IT IS NOT TOO LATE TO COME TO WASHINGTON! MAKE YOUR PLANS NOW! (for information write to info@thecuban5.org)
For more information about the Cuban 5 visit: http://www.thecuban5.org
II Annual "5 Days for the Cuban 5 in Washington DC" May 30 to June 5
To endorse: apoyojornada@gmail.com
Tags:dolores huerta, washington marriott wardman park
Posted in cuba-usa, human rights, medialies, solidarity, terrorism, The Cuban Five | 1 Comment »
PERSONALITIES AND ACTIVISTS CONVERGE ON WASHINGTON TO CALL FOR RELEASE OF THE CUBAN 5
International Committee for the Freedom of the Cuban 5 Announces
WELL-KNOWN PERSONALITIES AND ACTIVISTS FROM THE U.S. AND ABROAD TO CONVERGE ON WASHINGTON, D.C. TO CALL FOR A CHANGE OF US POLICY TOWARDS CUBA INCLUDING THE RELEASE OF THE CUBAN 5
CONTACT: Netfa Freeman, (202) 787-5229
(Spanish or English): Javier Rojo, (202) 787-5273
International Committee for the Freedom of the Cuban 5
info@thecuban5.org,
For a second time in two years, people from all over the U.S. along with members of parliament, lawyers and labor representatives from other countries will embark on a series of actions in the U.S. capital, beginning on May 30 and ending on June 5, to advocate for the release of the Cuban 5.
The Cuban 5 are five Cuban nationals who were accused and convicted of conspiracy charges against the United States. In fact, however, The Five's actions were never directed at the U.S. government. Their sole mission was to monitor Florida-based terrorist groups who had been relentlessly launching terrorist attacks against their country of Cuba. Activities of the week will include citywide outreach, public meetings, press conferences, a Hip Hop cultural event and several days of lobbying the Congress and Senate.
Partial list of participants in the five-day event series include Angela Davis, Father Miguel D'Escoto, former U.S. Attorney General Ramsey Clark, Ignacio Ramonet (former editor of La Monde Diplomatique), Dolores Huerta, Fernando Morais (Brazilian author), Danny Glover, Rev. Joan Brown Campbell, Saul Landau and many others.
On May 30, Father Miguel D'Ecosto, a former Foreign Minister of Nicaragua, will, along with other guests, hold a press conference at the National Press Club.
On June 1, buses from New York City, Quebec and other cities will be joining a significant number of Cuban Americans from Miami and activists from all over the U.S. at a rally in front of the White House to tell President Barack Obama: "Free the Cuban 5."
The "5 Days for the Cuban 5 in Washington D.C." was initiated by the International Committee for the Freedom of the Cuban 5 and sponsored by the Institute for Policy Studies (IPS). The International Committee is a network of concerned citizens from several countries of Europe, Latin America and the United States. The main objective of the International Committee is to raise awareness about the case of the Cuban 5.
For more information visit http://www.thecuban5.org,
Tags:attorney general ramsey clark, dolores huerta, joan brown campbell, politics
Posted in americalatina, changes in cuba, cuba-usa, human rights, medialies, solidarity, terrorism, The Cuban Five | 1 Comment »
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text:
Flashback #26
Posted by Just Another Film Buff under All Posts, Cinema of Germany, Flashback | Tags: Aguirre, Apocalypse Now, Forests in film, German Cinema, Klaus Kinski, Mind and movies, Peru, Ship on a tree, South America, Spanish invasion of South America, The Wrath of God, Werner Herzog |
Aguirre, Der Zorn Gottes (1972) (aka Aguirre: The Wrath Of God)
"I, the wrath of God, will marry my own daughter and with her I'll found the purest dynasty the earth has ever seen."
At the time when Rainer Werner Fassbinder was churning out a film in every two or three months, his contemporaries had to struggle to make a mark on the international arena. Things weren't any better for Werner Herzog, a budding director just two films old, with severe restrictions on the funds and large scale noncompliance from his crew. Yet, after all the distress before and during production, Herzog had survived and how. His third film, Aguirre: the Wrath of God, is seldom left out in any dissection of the German cinema history. Such was the impact of the film on the styles of the existing legends in the business.
The film is set in the sixteenth century when a large group of Spaniards, along with a army of slaves set out into the interiors of Southern America in search of the city of gold – El Dorado. At a point in their journey, the leader of the group decides to send further just a group of men who whose fate would decide the next move of the group. This team, consisting of Ursúa, Aguirre, his daughter, a team of soldiers and other vital persons, set out on limited resources, with no clue about the perils are about to face. Mentalities change, personal interests surpass the mission objective and savagery becomes the backbone of the agenda.
Each character in the journey has its own motivations to undertake it. The locals are fuelled by greed, the soldiers by fear, the priest by his religious ideologies and Aguirre by his own visions and narcissism. Aguirre – a man swallowed by his own ambitions – does not stop at anything and sacrifices everything for the attainment of the ultimate goal, much like Daniel Plainview of There will be Blood (2007) or Howard Hughes of Aviator (2004). Additionally, there are hints to argue that Aguirre believed himself to be placed in a superior race (a la Adolf Hitler) and it was his responsibility to fabricate a new world – a world ruled by the descendants, purely of his blood, even if that means an incestuous relationship with his daughter.
Herzog cleverly lets imagery take the driver's seat rather than verbalizing the complex diffusion and delirium of the mind. He uses the gorgeously lush yet singularly disturbing jungles and the seemingly clear stream to dictate the inner conflict of the titular character. As the stream grows wild and descends into the thick interiors of the savage forests, Aguirre's "obsession" escalates into the point of hallucination and even absolute detachment from reality. This innovative style of harnessing landscapes to underscore the characters' mentality would later be lapped up by Coppola in the extraordinary war epic Apocalypse Now (1979). Redoubling on the power of the imagery, Herzog also makes the film light on plot and dialogues. There is minimal conversation in the film and when it does appear, it makes a tremendous impact.
It is not rare that we see great films being made on a minuscule budget, for it is the fresh minds that bring in new ideas to the industry and are (hence) antonymous to sponsors. Aguirre, too, was made on a very small budget and the devastating filming conditions in the rainforests of Peru did no good. What is, perhaps, more interesting than the film itself is the hilarious and shocking bundle of tales behind its filming that deserves screen appearance, all by itself. Comparisons are unavoidable between Kinski and Aguirre himself and one does wonder how the pair worked for many more films after all that chaos during the shoot. Furthermore, it is stupefying how the team constructed shots such as the final one and the famous "ship on the tree" shot.
Aguirre: the Wrath of God is more of a psychological study of progressive insanity than an event oriented film. Its measured pace and direction induce a kind of trance into the involved viewer that one finds difficult to detach from. Do check out the Americanized version, Apocalypse Now, along with the film if you haven't. The twin films powerfully complement each other and reveal the influence of internal and external crises on the minds of men.
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text:
\section{INTRODUCTION}\label{sec:Introduction}

In the 30 years since its first demonstration \citep{Tyson90, Fort88},
 weak gravitational lensing has become an important tool for measuring the distribution of mass in the universe on scales ranging from galaxies
 \citep{Brainerd96, Fischer00}
 to large scale structure \citep{Abbott18, Hildebrandt16}.
Weak lensing has also provided increasingly precise measurements of the masses of clusters of galaxies
 (e.g. \citealp{Dahle02, Okabe10, Medezinski10, Umetsu14, vonderLinden14, Hoekstra15, McClintock19}).
A recent compilation of weak lensing observations \citep{Sereno15}
 includes 485 unique systems. For ground-based weak lensing observations,
 these studies have typically focused on clusters with $0.2<z<0.5$,
 in the optimal redshift range for maximizing the shear and signal to noise within a small ($\sim 10\arcmin$) region.

The availability of cameras with wider fields of view have enabled investigations of clusters at redshift $z <  0.1$ with comparable signal to noise.
However, study of these systems still lags behind the study of higher redshift systems.
For example, only $\sim 5\%$ (27 of 485) clusters used in \citet{Sereno15} are at $z < 0.1$.
Low redshift clusters are, however, important because they are easier to observe in detail with multiple techniques.
Many now have high-quality X-ray data and spectroscopic measurements of hundreds or even thousands of galaxies (e.g. \citealp{Sohn19a, Sohn19b}).

So far, weak lensing investigations of the lowest redshift systems, including the famous Coma Cluster \citep{Kubo07, Okabe14},
 use redshifts primarily to restrict the contamination of the weakly lensed source galaxies by unrecognized cluster members \citep{Okabe14}.
However, spectroscopy can play a much greater role in cluster mass measurements
 because biases in photometric redshift measurements are a dominant source of uncertainty in the weak lensing mass calibration \citep{vonderLinden14}.
On the basis of a Bayesian analysis of photometric redshifts for individual weakly lensed sources,
 \citet{Applegate14} make a strong case for the power of combining redshift surveys with weak lensing observations
 to suppress several of the systematics that impact cluster weak lensing results.

Here we demonstrate that combining weak lensing with deep, dense spectroscopy holds promise for direct evaluation and
 possible resolution of many subtle issues that affect the derivation of weak lensing cluster masses.
As a first example, we investigate the weak lensing signal for the massive system Abell 2029 ($z = 0.078$)
 based on a large, complete set of spectroscopic redshifts that includes background galaxies.
The low cluster redshift makes a sufficient number of weakly lensed sources accessible to
 the Hectospec instrument \citep{Fabricant05} mounted on the MMT 6.5 meter telescope.
This redshift survey provides a basis for direct calibration of the weak lensing signal,
 for evaluation of a weak lensing signal undiluted by cluster members,
 and for direct detection of superimposed background structures.

Because the majority of weak lensing studies make use only of photometric redshifts,
 there are increasingly sophisticated photometric approaches to the problems of contamination
 (both of the background galaxy sample and of the mass from superposition) and calibration of the photometric redshifts
 (e.g. \citealp{Medezinski07, Mandelbaum10, Applegate14, Hoekstra15, Umetsu16}).
These techniques have led to steadily improving limits on systematic biases.
Oddly, there has been no previous attempt to use a nearby cluster to measure
 the weak lensing signal based solely on a dense spectroscopic survey.

Our dense redshift survey of A2029 includes more than 5000 galaxies within $40\arcmin$ of the cluster center;
 the redshift survey is essentially complete to $r = 20.5$.
For the first time, we detect the cluster weak lensing signal.
Although the uncertainty in the mass calibration is large given the relatively smaller number of background galaxies with spectroscopic redshifts,
 the cluster mass we derive depends only on known geometric factors and does not depend on any external distance calibration.
Furthermore, the set of weakly lensed sources contains no cluster members.
Spectroscopy enables the use of all background galaxies in contrast with approaches that only include photometric sources fainter than a fiducial limit.
A2029 is a very rich system; the redshift survey robustly identifies cluster members.
We use these members to make two tests of potential weak lensing systematics.
In particular, we show that the B-mode (curl-like) shear signal from the cluster galaxies is consistent with zero
 at all projected distances from the cluster center.
The ``shear" signal from the cluster galaxies is also consistent (within $1\sigma$) with zero for cluster galaxies within $13\arcmin$ of the cluster center.
This absence of observed shear shows that there is no preferred orientation of cluster galaxies
 in agreement with \citet{Sifon15} and \citet{Lin17}.
The absence of a B-mode is also a test of systematics in the treatment of the point-spread function for the relatively bright objects we consider.

The A2029 system provides a measure of the weak lensing-induced ellipticity as a function of redshift (the ``tomographic" shear signal).
We base the measurement exclusively on sources with spectroscopically measured redshifts.
Although the uncertainties in the measure are large,
 the observed behavior is consistent with previously published mass estimates for A2029 \citep{Sohn19a}.

Several investigators have suggested a cosmological test
 based on the reduced shear as a function of redshift for a modest well-chosen set of clusters
 (\citealp{Medezinski11}; Figure 1 of \citealp{Applegate14}).
The A2029 experiment demonstrates the feasibility of a cosmological test based on much larger, deeper, redshift surveys of well chosen
 sets of clusters carried out with future instruments like Subaru/Prime Focus Spectrograph (PFS, \citealp{Tamura16})
 or GMT/GMACS \citep{DePoy18}.

In Section~\ref{sec:Phot}, we describe the photometric data acquisition and reduction used to produce the object catalog and to derive the ellipticities of the objects.
In Section~\ref{sec:Spectra}, we describe the spectroscopic data.
In Section~\ref{sec:Shear}, we describe the ellipticity measurements for the objects with spectroscopic redshifts.
In Section~\ref{sec:Profile_Tomography}, we derive the ellipticity profile versus projected radius and the tomographic measurements.
Finally, in Section~\ref{sec:Discussion}, we discuss the spectrotomographic detection and the prospects for exploiting
 the combination of weak lensing shear and spectroscopic redshifts with upcoming massively multiplexed fiber instruments to make sensitive cosmological predictions.

\section{Photometric Data analysis and catalog generation}\label{sec:Phot}

\subsection{Photometric Data and Processing}\label{subsec:imagedata}

Photometric observations were taken with the Dark Energy Camera (DECam) at the Cerro Tololo Inter-American Observatory's 4-meter telescope.
The DECam imager consists of 62 2048 $\times$ 4096 pixel science CCDs (60 of which are currently operational) arranged in a hexagon.
DECam images cover 2.2 square degrees at a 0\farcs265/pixel scale \citep{DePoy08, Flaugher15}.

The A2029 data for this project were obtained during four observing runs (04/26-28/2013, 06/11-16/2013, 08/29-31/2014, 03/30-04/02/2014).
The data were obtained as part of two separate observing programs: a dedicated campaign by Jacqueline McCleary to look for cluster substructure,
 and a DECam program by Anja von der Linden to obtain scaling relations for cluster cosmology.
The observations cover  five filter bands ($ugriz$), to allow photometric redshift calculation.
For our analysis, we only make use of data in the filter band with the best seeing ($i$).
Observations were taken as sequences of dithered exposures (each typically 120s or 300s).
Only exposures taken in seeing better than $1\arcsec$ were used in the shape analysis.
The final exposure time for these ``good-seeing''$i$-band observations was 4920 seconds.

Instrumental signatures were removed using the DECam Community Pipeline (CP).
The CP performs: bias calibration; crosstalk; masking and interpolation over saturated and bad pixels;
 CCD non-linearity and the flat field gain calibration; fringe pattern subtraction; astrometric calibration;
 single exposure cosmic ray masking; characterization of photometric quality; sky pattern removal; and illumination correction.
For full descriptions of the DECam pipeline processing system, see chapter 4 of the NOAO Data Handbook~\citep{NOAODHB2.2}.

\subsection{Image Stacking and Calibration}\label{subsec:photometry}

We base our analysis of the deep lensing-quality image in \citet{MDvdL_2018}.
For convenience, we summarize the steps leading to this image.

\citet{MDvdL_2018} create the stacked image using a weighted stacking algorithm.
They calculate weights for the individual exposures based on their photometric depth,
 obtained by matching instrumental magnitudes of unsaturated stars to those in the Sloan Digital Sky Survey (SDSS) Data Release (DR) 12 catalog \citep{Alam15}.

They resampled individual scaled exposures onto a common astrometric grid and combined them into a stacked image using {\sc SWarp}~ \citep{Bertin10}
 which also performs the sky subtraction on the individual exposures allowing for a uniform sky even in the presence of uneven weights
 due to gaps and defects in individual exposures.
For the projection step, \citet{MDvdL_2018} use \texttt{Lanczos3} kernel, chosen because of its robust noise-conservation properties and computational efficiency.

To produce the final image, \citet{MDvdL_2018} use the clipped mean extension to {\sc SWarp}.
This approach is exceptionally stable to a wide range of artifacts in individual frames and
  produces a stacked image where the point-spread function (PSF) is a linear combination of the single frame PSFs \citep{Gruen14}.
Thus the clipped mean stacks are well-suited for weak lensing shape measurement.
In addition to the lensing stack, \citet{MDvdL_2018} produce a photometry-quality stack
 (a deeper image made from all exposures with FWHM less than 1.5 arcseconds) for each imaging band.
We only use the lensing stack image for the weak lensing analysis.

To test whether the image stacking process introduced significant ellipticity correlations,
 we use the stellar PSF shapes along with the correlation between the residual stellar ellipticities and those of the galaxies.
We begin by identifying a sample of bright but unsaturated star catalogs using the size-magnitude relation for all objects.
We use these stars to characterize the PSF in terms of its size and second moment.
We measure the PSF anisotropy $\boldsymbol{q^\star}=(P^{\star sm})\boldsymbol{e^\star}$ at the location of each star,
 and interpolate the variation of the anisotropy across the field of view using a simple polynomial model.
The best order of polynomial fit is derived from the same 10-fold cross-validation technique discussed in Weighing the Giants (WTG1, Appendix B of \citealp{vonderLinden14}) and summarized here.
First, we randomly subdivide the stars used for PSF correction into 10 groups.
For each group, we compute ellipticity residuals compared with the polynomial fit to the stars in the other nine groups.
This technique yields an estimate of the PSF ellipticity residuals at the location of every star without using that star in the fits.
We choose the polynomial order which minimizes the sum of the standard deviations of the two ellipticity components $e^\star_1$ and $e^\star_2$ as the best fit.
We apply this correction to all objects in the catalog.
The large size of the DECam field of view means that the PSF variation in the A2029 field is best captured by an 8th-order polynomial.
Although this high order corresponds to a significant freedom in fitting,
 the fit is constrained by the measured shapes of $\sim 10^4$ stars.
Residual PSF errors after the fit are $\ll 0.5$\%
 on angular scales larger than $1\arcmin$ over the central $1.5^{\prime}$ of the field.

PSF errors over the angular region we consider (within 23$^{\prime}$ of the cluster center) do not contribute significantly to the shear measurement errors.
In Section \ref{sec:Shear} we use the combined PSF-corrected image for the weak lensing analysis.

\section{Spectroscopic Data}
\label{sec:Spectra}

\citet{Sohn19a} carried out a dense and complete spectroscopic survey of A2029.
Within $30^{\prime}$ of the cluster center, the redshift survey is 90\% complete to $r = 20.5$.
We use the redshifts to identify cluster members and foreground/background galaxies.
The background redshifts are the basis for the spectroscopic tomography.

To construct the complete spectroscopic survey,
 we first collected redshifts of  bright A2029 galaxies from the SDSS
The SDSS acquires the spectra for galaxies brighter than $r = 17.77$ through $3\arcsec$ fibers.
There are 681 objects with SDSS spectra within $40\arcmin$ of the cluster center.
The typical redshift uncertainty for SDSS spectra is $13~\rm km~s^{-1}$.

We also collected redshifts of 41 A2029 galaxies from the literature (e.g. \citealp{Bower88, Sohn17}),
 accessed through the NASA/IPAC Extragalactic Database (NED).
\citet{Tyler13} measured redshifts of A2029 galaxies using Hectospec mounted on MMT 6.5m telescope,
 a fiber-fed spectrograph that obtains $\sim 250$ redshifts over an $\sim 1~{\rm deg}^{2}$ field of view \citep{Fabricant05}.
We collected 1362 redshifts from \citet{Tyler13} through the MMT archive \footnote{http://oirsa.cfa.harvard.edu/archive/search/}.

We then conducted a denser, more complete redshift survey of A2029 using MMT/Hectospec \citep{Sohn17, Sohn19a}.
The survey targets are galaxies with $r_{\rm petro} = 21.3$ and $r_{\rm fiber} = 22$ in the SDSS photometric galaxy catalog.
We imposed the fiber magnitude selection to exclude low surface brightness galaxies from the target list.
There is no color selection for survey targets.

For the Hectospec observations , we used the 270 line mm$^{-1}$ grating also used by \citet{Tyler13}.
The resulting spectra have a resolution of 6.2~{\rm \AA} covering a wavelength range $3700 < \lambda < 9150$ {\rm \AA}.
We observed each field with three exposures of 1200 seconds to allow for cosmic ray removal.

We used the HSRED v2.0 IDL package to reduce the Hectospec spectra.
We derive the redshifts using the RVSAO \citep{Kurtz98} package that
 cross-correlates Hectospec spectra and a set of template spectra prepared for this purpose \citep{Fabricant05}.
We visually inspected the reduced spectra and divided the results into three categories:
 `Q' indicates a high-quality redshift, `?' an ambiguous result, and `X' denotes a poor quality redshift.
We use only the 2890 high-quality redshifts.
The typical redshift uncertainty for Hectospec spectra is $\sim 29~\rm km~s^{-1}$.

A2029 is one of the best-sampled galaxy cluster fields.
Within $30^{\prime}$ of the cluster center defined by the brightest cluster galaxy (BCG),
 IC1101, there are 3568 objects with measured redshifts.
The spectroscopic completeness is $\sim90\%$ to $r < 20.5$ within $R_{cl} < 30\arcmin$ ($\sim 67\%$ to $r < 21.3$).
The spectroscopic survey is uniform within $R_{cl} < 30 \arcmin$ (see Figure 1 in \citealp{Sohn19a}).

\begin{figure}
\centering
\includegraphics[scale=0.4]{A2029_cone.eps}
\caption{Cone diagram of the A2029 field projected in the R.A. direction.
Gray points are the galaxies with a spectroscopic redshift.
Green points are spectroscopically identified members of A2029.
Red and blue points are galaxies within $R < 13\arcmin$ and $R < 23\arcmin$, respectively.
We use these galaxies at $z > 0.1$ for the weak lensing analyses. }
\label{fig:A2029cone}
\end{figure}

Figure \ref{fig:A2029cone} shows a cone diagram for the entire redshift survey.
The finger corresponding to A2029 is obvious at mean redshift of 0.078.
The voids and filaments characteristic of the large-scale structure of the universe are evident particularly in the background.
There is also foreground structure which we use below to test the robustness of the lensing signal.
We highlight the two radial ranges where we explore the weak lensing signal:
 the blue points highlight objects within the approximate virial radius, $R = 23 \arcmin$.
We highlight the dense central region of the cluster (R $ < 13\arcmin$) in red.

We use the total redshift survey to  identify cluster members and foreground/background objects.
We identify cluster members using the caustic technique \citep{Diaferio97, Diaferio99, Serra13},
 a non-parametric characterization of the cluster boundary.
The caustic technique estimates the boundary of clusters in the phase space,
 the relative velocity difference with respect to the cluster mean velocity as a function of cluster-centric distance. We identify
galaxies within the cluster boundary phase space
as cluster members (see Figure 4 in \citealp{Sohn19a}).

Table \ref{tabstat} summarizes the various subsets of the spectroscopic sample relevant for the spectroscopic tomography.
The table includes the number of galaxies with both a redshift and an ellipticity measurement that are cluster members,
 foreground galaxies, or background objects
 within two projected radii ($13\arcmin$ and $23\arcmin$) of the cluster center defined either by the weak lensing map or by the position of the BCG.
We use the samples of background galaxies with redshifts and ellipticities for the spectrotomographic measurements.

\begin{deluxetable}{lccccc}
\label{tabstat}
\tablecolumns{6}
\tabletypesize{\scriptsize}
\tablecaption{A2029 Redshift Samples}
\tablehead{
\multirow{2}{*}{Type}	& \multicolumn{2}{c}{WL Center} & &  \multicolumn{2}{c}{BCG} \\
										& $R < 13'$ & $R < 23'$ & & $R < 13'$ & $R < 23'$}
\startdata
Spec. objs											& 859	& 2252 &	&	860	&	2256	\\
Spec. objs with shear measurements	& 854	& 2225 &	&	855	&	2228	\\
Spec. member									& 339	&	595	&	&	338	&	597	\\
Spec. foreground								& 46		&	100	&	&	46		&	99		\\
Spec. background								& 474	& 1517	&	&	466	& 1519	\\
Spec. background, $z > 0.10$			& 433	& 1431	&	&	426	& 1432	\\
\enddata
\end{deluxetable}

\section{Weak Lensing Shear Measurements}
\label{sec:Shear}

Weak lensing shear measurements require fitting for and subtracting the effect of the PSF on the galaxy shapes.
Several methods have been developed to extract the the PSF-corrected ellipticity components
 ({\it e.g.} KSB \citep{Kaiser95}, Bernstein \& Jarvis \citep{Bernstein02}).
We use the well-established ``Regaussianization'' technique of Hirata, Seljak and Mandelbaum (HSM) \citep{Hirata04, Singh15}.

We use the implementation of HSM included in the LSST Software data management system (the LSST Science Pipelines).
This implementation is also used in analyzing the Subaru Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) survey \citep{Mandelbaum18, Hikage19}
 both for PSF-modeling and shape fitting.
To access these algorithms, we use the {\it obs\_file} package \footnote{https://github.com/SimonKrughoff/obs\_file}
 which allows running of the core LSST analysis packages on individual stacked images.
We use the stacked image produced in Section \ref{sec:Phot} as the input for the shape measurement.
We cross-correlate the output catalog with the spectroscopic catalog.
The imaging catalog detects about 1.2 million objects (mostly galaxies in the A2029 field with significance greater than $5\sigma$;
 almost all of these galaxies are fainter than the spectroscopic limit).
Because source crowding is an issue, we use the built-in deblending algorithm in DMStack
 to separate sources and to measure shapes for the deblended objects.
We select only objects without deblended sub-objects ($N_{child}=0$).
This selection could bias the photometry for the largest galaxies in our sample.
However, we do not rely on this photometry when matching our sources to the spectroscopic sample;
 we rely only on centroid positions.
We use the HSM-derived ellipticity components ($e_1$, $e_2$) to calculate the tangential ellipticity profile and the tomographic signal for A2029.

Because of differences in deblending close neighbors and source multiplicity,
 not every spectroscopically measured object has an HSM-measured shape.
Table \ref{tabstat} lists
 the relevant numbers of spectroscopic objects and spectroscopic objects with shapes
 for each subsample we analyze.
All of the objects without shapes are either stars ($\sim 53$\%),
 cluster members ($\sim 12$\%) or foreground objects ($\sim 35$\%).

\citet{MDvdL_2018} demonstrate a statistically significant weak lensing signal $R = 23\arcmin$ of the lensing center.
We thus restrict the subsequent analysis to galaxies within this radius.
The position of the highest lensing peak in \citet{MDvdL_2018} is offset by about $0.3\arcmin$ from the center of the BCG, IC1101.
Table \ref{tabstat} gives the numbers of objects in samples centered on
 the weak lensing peaks and on the BCG.
In Section \ref{subsec:Qchecks}, we show that these two choices of the lensing center have minimal overall impact on the spectrotomographic signal.

\subsection{Weak Lensing Measurement}

In weak gravitational lensing,
 the distortion of the images is described by the reduced shear $\boldsymbol{g} =\frac{\boldsymbol{\gamma}}{1-\kappa}$,
 where $\boldsymbol{\gamma}$ represents the anisotropic shear induced in the galaxy images.
The reduced shear is a function of the projected mass density of the lens.
At fixed lens redshift, the reduced shear is a function of the source redshift through the angular diameter distance ratio ${D_{\rm ls}\over D_{\rm s}}$,
 which impresses a characteristic pattern on the lensing signal as a function of source redshift.
For a low redshift cluster like A2029, the tomographic lensing signal is a steep function of redshift for $z>z_{cluster}$ (Figure \ref{fig:dratio}).

\begin{figure
\centering
\includegraphics[scale=0.4]{A2029_wl_dratio.eps}
\caption{The angular diameter distance ratio ${D_{LS}/D_S}$
 as a function of source redshift for galaxies behind A2029.
Distances assume a $\Lambda$CDM cosmological model
 with $\Omega_m=0.27$ and $\Omega_\Lambda=0.73$. }
\label{fig:dratio}
\end{figure}

The reduced shear is related to the measured {\it tangential ellipticity}:
\begin{equation}
e_{\tan} = -(e_1 \cos(2\phi) + e_2 \sin(2\phi)) \simeq 2\gamma \label{eqn:etan}.
\end{equation}
The variables $e_1$ and $e_2$ in Equation~\ref{eqn:etan} are
 the polarization states of background galaxies with complex ellipticities $\boldsymbol{e}$,
 measured in terms of the image axes $x$ and $y$;
 $\phi$ is the azimuthal angle between the $x$-direction and the vector
 connecting the position of the center of the cluster's mass to the position of the galaxy.

\subsection{Expected Signal Extent}

According to \citet{MDvdL_2018} the distortion effects of A2029 are significant within $R = 23\arcmin$.
\citet{MDvdL_2018} selected background galaxies based on their photometric redshifts.
They selected galaxies with photometric redshift probability $P (z  >0.19) > 0.8$
  based on BPZ template-fitting \citep{Benitez00}.
Although this procedure largely selects background galaxies,
 there is significant cross-contamination of the background by faint cluster members.
However, the photometric sample still provides a robust extent of the shear signal.

Figure 16 of \citet{MDvdL_2018} shows that tangential shear for the photo-z sample is detected
 at high signal to noise (and with reduced shear ${\bf g} > 0.01$) to a radius $R=23\arcmin$,
 approximately the virial radius for A2029 \citep{Sohn17}.
Although that  sample contains some cluster members,
 the large number of galaxies used in the photometric shear measurement leads to
 a higher S/N measurement of the lensing signal than
 we can obtain for the spectroscopic measurement described below.
For this reason, we use $R < 23\arcmin$ as the radial extent over which
 we measure the signal for the spectroscopic sample.

\subsection{Quality Checks}
\label{subsec:Qchecks}

Systematic tests on the residual PSF ellipticities in the lensing image were already carried out in \citet{MDvdL_2018}.
We perform additional tests on the shape catalog to verify that systematic errors that could mimic a shear signal are inconsequential.
Additionally, we  use  the ``B-mode" or curl-like component of the ellipticity tensor to verify that the signal has the characteristics of genuine lensing.

\subsubsection{Ellipticity Component Distributions for the Photometric Sample}

In the absence of systematic errors (and in the limit where ${\bf g} \ll 1$)
 the tangential ellipticity is an unbiased estimator of the reduced shear when averaged over galaxies.
As a test for systematic offsets in the galaxy shapes,
 we plot the distribution of ellipticity components $e_{1}$ and $e_{2}$
 (corresponding to the ``plus" and ``cross" pattern ellipticities)
 for galaxies in the HSM catalog for the A2029 field.
In the absence of systematic distortions,
 the azimuthal symmetry of the vectors to the center of A2029 should result in
 indistinguishable distributions $N (e_{1})$ and $N (e_{2})$ even in the presence of a lensing signal.
The upper panel of Figure \ref{fig:A2029_shear_distribution} shows that
 the two distributions are similar:
 the lower panel shows $(N(e_{1}) - N(e_{2})) / (N(e_{1}) + N(e_{2}))$ as a function of ellipticity.
The differences are within the 1$\sigma$ errors throughout the ellipticity range.
The largest excursions at the extreme values of ellipticity in the bottom panel occur
 because there is a negligible number of objects with that ellipticity.

\begin{figure}
\centering
\includegraphics[scale=1.0]{A2029_wl_ellip.eps}
\caption{(Top) Distribution of HSM ellipticity estimates $e_1$ and $e_2$ for
 the A2029 spectroscopically matched shape catalog within $R = 23\arcmin$.
(Bottom) The differential ratio between $e_{1}$ and $e_{2}$ as a function of ellipticity.
There is no statistically significant preferential residual offset between the ellipticity components.
}
\label{fig:A2029_shear_distribution}
\end{figure}

\subsubsection{Tangential and ``B-mode" distribution for the Sample with Redshifts}

In the presence of lensing,
 the distributions of $e_{cross}$ and e$_{tan}$ should differ with a systematic offset
 towards non-zero values of $e_{tan}$.
The upper panel of Figure \ref{fig:etanecrosshist} shows histograms of the numbers of galaxies
 with a given value of tangential ellipticity ($N_{etan}$) and
 the number of galaxies with the same value of the cross (or B-mode) ellipticity ($N_{ecross}$).
The lower panel of Figure \ref{fig:etanecrosshist} shows
 the expected offset between the two distributions.
We restrict the sample of objects to those within $R = 23 \arcmin$ and with $z > 0.1$.
A Kolmogorov–Smirnov (KS) test demonstrates that the distributions in the upper panel are inconsistent with being drawn from
 the same underlying distribution at a level $p = 0.0005$.
The Anderson-Darling (AD) test gives a similar result.
In essence the statistical significance given by the KS and AD tests is
 our first measure of the significance of the spectroscopic tomographic signal.
The offset between the two distributions is the mean lensing-induced tangential ellipticity.

We can also examine the difference between the two distributions in Figure \ref{fig:etanecrosshist}
 as a function of ellipticity to check for systematic bias in the spectroscopic sample selection.
We can approximate the two offset distributions as Gaussians
 with the width of the ellipticity distributions.
If the lensing signal were caused by a selection bias in the spectroscopic selection,
 the signal would originate primarily from galaxies with large tangential ellipticities.
This effect is absent in Figure \ref{fig:etanecrosshist}.
In fact, the pattern of tangential ellipticities matches the theoretical expectation very closely.
This test demonstrates the importance of {\it complete} redshift surveys for avoiding bias in lensing measurements.

\begin{figure}
\centering
\includegraphics[width=0.9\columnwidth]{A2029_wl_dellip.eps}
\caption{(Top) Distribution of tangential ellipticity $e_{tan}$ (red) and ``B-mode"  ellipticity $e_{cross}$(black)  for
 the A2029 field galaxies within $R = 23\arcmin$ at $z > 0.1$ (A2029 background galaxies).
(Bottom) The difference between the $e_{tan}$ and $e_{cross}$ distributions (in the upper panel) as a function of ellipticity.
The superimposed curve shows the theoretical expectation for two normal distributions offset
 by the mean shear signal observed for A2029. }
\label{fig:etanecrosshist}
\end{figure}

\subsubsection{Choice of Cluster Center}

Because we calculate the tangential and cross ellipticity components for each galaxy
 with respect to the direction between the galaxy and the center of the cluster,
 the choice of center could significantly affect  the measured tangential shear pattern (see Equation \ref{eqn:etan}).
To test the impact of the choice of center, we compute the spectrotomographic signal
 using two different centers, the weak lensing peak \citet{MDvdL_2018} and the position of the BCG (see Table 1).

These two centers are within $0.3\arcmin$ of one another.
Figure \ref{fig:comparecenters} thus shows that the lensing signals are very similar.
In each bin, the tangential ellipticities are consistent within the uncertainties and the overall normalization is also similar.
On average, the lensing signal is $\sim 5\%$ lower
measured with respect the center of IC1101 rather than with respect to the lensing signal.
It is perhaps not surprising that the weak lensing center maximizes the signal, but the effect is small.
In the following analysis we use the weak lensing center.

\begin{figure}
\centering
\includegraphics[width=0.7\columnwidth]{A2029_wl_center.eps}
\caption{The spectrotomographic signal for the $23 \arcmin$ sample with two different cluster centers.
In all bins, the signals are within the $1\sigma$ uncertainties,
 but the overall normalization of the signal depends very slightly on the choice of center. }
\label{fig:comparecenters}
\end{figure}

\subsubsection{Cluster Members and Foreground Galaxies}

In principle, the shear and B-mode signals for the cluster galaxy sample test models of the intrinsic alignment of cluster galaxies (e.g. \citealp{Kiessling15, Huang18}).
We use the caustic pattern of A2029 to select cluster members (see Section \ref{sec:Spectra}).
We can then compute the shear signal separately for cluster members and for unrelated foreground galaxies.
There are 597 caustic-selected cluster members within a projected distance of $23\arcmin$
 of the center of A2029 (338 within $13\arcmin$).
For these cluster galaxies the mean tangential ellipticity is consistent with zero to
 within $1\sigma$ ($0.014\pm 0.017$) for the $13\arcmin$ sample.
This result implies that intrinsic alignment is unimportant as suggested by other studies.
The mean tangential ellipticity is larger in the larger radius sample;
 it is marginally inconsistent with zero at $2.2\sigma$ ($0.030\pm 0.014$).
This result is inconsistent with a model where intrinsic alignments result from
 galaxy interactions \citep{Singh15}
 and may indicate some unknown source of correlation in cluster galaxy orientations.
The B-mode signal for cluster members is consistent with zero ($1\sigma$ negative) for
 both 13 and $23\arcmin$ samples.

There are 101 foreground galaxies within $23 \arcmin$.
These objects obviously should not be lensed.
Both the  ``shear" signal and the B-mode from these galaxies is consistent with zero.
The mean tangential ellipticity is $-0.014\pm 0.023$, and the B-mode signal is $0.025\pm 0.023$.
The signal from the 698 galaxies within $23 \arcmin$ and including cluster members and the foreground is insignificant.

The uncertainty in the measurement from this single cluster is too large
 to distinguish among models which predict positive and negative tangential alignments.
However with deep cluster samples of the future that could reach 3 magnitudes
 deeper than the survey we use, the number of cluster member would increase by
 a factor of 10 or more depending on the faint end slope of the luminosity function (LF, \citealp{Sohn17}).
The number we quote refers to a flat faint end; a steep faint end (e.g. \citealp{Agulli16})
 only increases the number.
Uncertainties based on these large samples will be
 a factor of $\sim4$ smaller thus providing powerful constraints on model predictions.

\section{Shear Profiles and Tomography}\label{sec:Profile_Tomography}

\begin{figure*}
\centering
\includegraphics[scale=0.6]{A2029_wl_tomography.eps}
\caption{Azimuthally averaged mean tangential ellipticity (red circles) and cross ellipticity (blue squares)
 as a function of spectroscopic redshift  for A2029
 within (Left) $R = 13\arcmin$ and (Right) $R = 23\arcmin$.
The data point at the lowest redshift is the average signal from the union of the cluster members and foreground galaxies.
Bins at redshift greater than that of A2029 cover the ranges $0.1<z<0.3$, $0.2<z<0.4$, $0.3<z<0.6$, $0.4<z<0.7$, and $0.5<z<0.8$.
The curve shows the expected signal for a $c=4$ NFW cluster with $M_{200}=9\times 10^{14} M_\odot$, corresponding to the X-ray derived mass from \citet{Walker12, Sohn19a},
with angular diameter distance scaling derived from actual distribution of spectroscopic redshifts within the bin. }.
\label{fig:tomography}
\end{figure*}

Figure \ref{fig:tomography} shows the mean azimuthally averaged tangential (and cross-) ellipticity in different redshift bins.
The bin for $z < 0.1$ includes the union of the caustic-selected cluster galaxies and foreground galaxies.
The gray background indicates that this point does not enter the shear computation.

Higher redshift bins cover the ranges
 $0.1 < z < 0.3$, $0.2 < z < 0.4$, $0.3 < z < 0.6$, $0.4 < z < 0.7$, and $0.5 < z < 0.8$.
We calculate the tomographic signal both for the sample of galaxies
 within a radius of $23\arcmin$ of the center of A2029 (left),
 and for a radius of $13\arcmin$ (right).
We choose these radii because
 $23 \arcmin$ is the approximate virial radius of the cluster \citep{Sohn19a} and
 $13 \arcmin$ corresponds to a projected radius of 1 Mpc.
The choice of the 1 Mpc radius is dictated by a balance
 between the expected signal amplitude and the number of sources with a redshift.
For all bins, the B-mode ellipticity is consistent with zero within $\sim 1\sigma$,
 except for the $23\arcmin$ at $0.3<z<0.5$ bin,
 where it is approximately $2\sigma$ positive.
This single marginally significant departure is not a serious concern.

We superimpose the expected mean tangential ellipticity
 (scaled to the mean angular diameter distance of the galaxies)
 in each bin for a cluster modeled as an NFW with $c=4$ and $M_{200} = 9 \times 10^{14} M_{\odot}$,
 in accordance with the X-ray derived mass in \citet{Sohn19a}.
We emphasize that we do not fit the curve to the data points to derive a best-fit NFW model.
Given the S/N of our detection, the uncertainty would too great.

We calculate the significance of the detection of
 a shear signal by constructing $10^{6}$ realizations of the shape catalog
 using randomly oriented galaxies with the distribution of ellipticities in the real catalog.
Furthermore, we divide the galaxies into
 different redshift bins as in Figure \ref{fig:tomography},
 and repeat the random realizations in each bin.
Thus, we reject random realizations with large positive signal at low redshift.
There are 51 (117) realizations exceeding the measured signal within $23\arcmin$ ($13\arcmin$)
 corresponding to $3.9\sigma$ ($3.7\sigma$).
These values measure the significance of the detection of the lensing signal from A2029.

Although the $23\arcmin$ sample is slightly more significant,
 the detection significance is not strongly dependent on the area sampled;
 the same pattern is evident in both samples.
The amplitude of the mean tangential ellipticity signal for galaxies
 projected closer to the center of A2029 shows a larger shear signal (as expected).
This result shows the power of the spectroscopy which segregated the global signal of
 Figure \ref{fig:tomography} as a function of redshift.
This detection is the first tomographic lensing signal for a cluster
 based exclusively on galaxies with actual spectroscopic redshifts;
 it is the first spectrotomographic detection.

The difference in overall signal level in the left and right panels of Figure \ref{fig:tomography}
 demonstrates that, as expected,
 there is a measurable radial gradient in the tangential ellipticity.
We plot the tangential ellipticity versus radius for all galaxies with $z_{spec} > 0.1$
 in the right panel of Figure \ref{fig:tangentialshear_withredshiftg0.3}.
The overplotted curve again corresponds to an NFW profile of tangential ellipticity
 expected for a cluster with $M_{200}=9.0\times 10^{14} M_{\odot}$ and $c=4$,
 scaled for the mean angular diameter distance ratio for the sample
 (a great advantage of a spectroscopic redshift sample is that the distance ratio scaling can be calculated exactly).
The radial profile behaves roughly as expected.
This exercise demonstrates that the tomographic signal
 we detect is not driven by small-scale features in the distribution of galaxy shapes.

The radial ellipticity profiles in Figure \ref{fig:tangentialshear_withredshiftg0.3}
 also provide additional evidence that the shapes are unbiased.
A radially-dependent bias would show up as a constant additive offset
 in the mean tangential ellipticity at all redshifts.
The lack of systematic offset in the cluster and low-redshift bins shows that
 the spectroscopic selection does not bias the resulting lensing calculation.
Including only galaxies that are spectroscopically confirmed to be behind the cluster
 leads to an increased shear signal compared with
 the signal from the photometric sample of \citep{MDvdL_2018}.
This behavior again highlights one of the strengths of a spectroscopic sample;
 there is no calibration required to correct for the unknown distribution of
 angular diameter distance ratios.

\begin{figure}
\centering
\includegraphics[width=0.95\columnwidth]{A2029_wl_zbin.eps}
\caption{Azimuthally averaged tangential ellipticity (and cross ellipticity)
 as a function of radius from the center of A2029 for galaxies with measured spectroscopic redshifts.
(Left) The tangential and cross ellipticity profile for galaxies in and in front of the cluster,
  which should not show any gravitational lensing signal.
(Right) The tangential and cross ellipticity profile for galaxies with $0.1< z <0.8$.
The curve is the NFW profile for a cluster with $M=9.0\times 10^{14} M_{\odot}$, $c=4$,
 scaled to the mean angular diameter distance ratio for the spectroscopic sample.}
\label{fig:tangentialshear_withredshiftg0.3}
\end{figure}

\section{Limitations and Future Surveys}
\label{sec:Discussion}

We detect the tomographic weak lensing signal from the massive cluster A2029
  using only spectroscopically confirmed background objects.
The factor limiting the signal-to-noise of the detection is not the ability to measure shears.
These  measurements are now relatively easily acquired for galaxies
 behind dozens of galaxy clusters and data for hundreds more will be readily available
 thanks to ongoing and upcoming surveys with HSC and LSST.

The main limitation is the  availability of deep, dense redshift surveys.
We detect the signal for A2029 because it is a very massive cluster,
 and because its redshift is low enough that a dense redshift survey complete to $r \sim 20.5$
 includes enough background galaxy redshifts.

With the imminent arrival of wide-field spectrographs on large telescopes
 such as Subaru/PFS \citep{Tamura16} and subsequently of GMACS on the GMT \citep{DePoy18},
 much larger redshifts surveys reaching to much fainter magnitudes
 will be feasible with reasonable telescope time allocations.
Our experiment demonstrates that
 these observations will lead to high-significance measurements of individual clusters,
 opening observational techniques of spectrotomography
 as a probe of cluster mass distributions and cosmology \citep{vonderLinden14, Hoekstra15, McClintock19}.

As an example of the power of these observations,
 we consider galaxy cluster measurements achievable with PFS.
We model the tomographic signals  achievable with a PFS survey complete to $i=22.7$ (corresponding to $\sim 1.5$ hour of exposure per cluster) or $i=23.7$ corresponding to 6 hours/cluster.
To estimate the number of resolved targets within our $23\arcmin$ radius field,
 we use the galaxy source density derived from deep, high-quality ($\sim 0.5\arcsec$)
 seeing imaging of the F2 field \citep{Utsumi16}.
This photometric sample represents a more typical image quality for future source selection than
 the A2029 data itself.
We use the measured source counts in F2 to construct two catalogs,
 one representing a selection complete to $i<22.7$ (6540 galaxies),
 and one complete to $i<23.7$ (14510 galaxies).

For each galaxy in a catalog,
 we assign a redshift based on the distribution of photometric redshifts versus magnitude
 from \citet{Ilbert09}.
Next, we assign the galaxy a cross ellipticity drawn from
 a zero-centered distribution with a dispersion equal to the dispersion in our measured $e_{1}$,$e_{2}$ distributions for A2029.
We also assign a tangential ellipticity given by the model for an NFW cluster with $M=9.0\times 10^{14} M_{\odot}$.
The dispersion of a mean tangential ellipcitiy is the same as for the cross ellipticity (see Figure \ref{fig:etanecrosshist}).

We use those distribution of redshifts and simulated ellipticities to construct realizations of tomographic measurements with PFS.
Figures \ref{fig:pfs23} and \ref{fig:pfs24}, respectively, show realizations of
 the spectrotomographic measurements for a single realization complete to $i=22.7$ and $i=23.7$.
For each realization, we calculate the signal-to-noise of the detection of the tomographic signal,
 extending our calculation to include redshift bins out to $z=1.5$.

Note that, in addition to the reduction of the error bars in the redshift range explored in this work,
 a PFS survey would extend the redshift distribution of the background sources out to $z \ge 1.5$.
The result is an impressive increase in the detectability of the tomographic signal at high redshift.

The typical simulated PFS survey to $i<22.7$ reaches a signal-to-noise ratio of
$\sigma=7.4$; the $i<23.7$ survey reaches $\sigma =11.7$.
These results are comparable to the significance reached by
 current photo-z based lensing cluster measurements.

Carrying out these surveys with PFS would be straightforward, given the 2400-fiber multiplexing.
Carrying out a survey complete to $i=22.7$ requires $\sim 4$ hours of exposure per cluster.
A survey complete to $i=23.7$ would obviously be slower; each cluster would take $\sim 2.5$ nights.
The observations would also be extremely valuable for the study of the star formation and the stellar content cluster galaxies and of the field galaxy populations at intermediate redshift.
Potentially samples of $\sim 50$ clusters could be observed even to $r=24$,
 allowing measurement of the slope of the angular diameter distance ratio to
 $(d{\bf \gamma}/ dz) \sim 0.1$ to a redshift of 1.5.

\begin{figure}
\centering
\includegraphics[width=0.7\columnwidth]{A2029_wl_pfs23.eps}
\caption{Azimuthally averaged tangential (and cross) ellipticity for galaxies as a function of redshift,
 for a single realization of a model PFS survey.
The model galaxies are within $i=22.7\arcmin$ of the center of A2029.
The galaxy counts  are based on Subaru HSC $0.5 \arcsec$ imaging \citep{Utsumi18} and
 reshifts from zCOSMOS \citep{Ilbert09}.
We assume the mean tangential ellipticity from a pure NFW model for the cluster assuming the dispersion in ellipticities matches that of the e$_{1}$ and e$_{2}$ distributions we observe }
\label{fig:pfs23}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.7\columnwidth]{A2029_wl_pfs24.eps}
\caption{Simulation of a PFS survey complete to $i=23.7$, with the same assumptions as in Figure \ref{fig:pfs23}. }
\label{fig:pfs24}
\end{figure}

PFS (and eventually the multi-object spectrographs on giant telescopes) will enable weak lensing measurements
 based on purely spectroscopic samples of background galaxies with comparable precision to those
 currently made with photometrically selected samples.
Larger telescopes will enable these measurements for clusters at larger redshift.

Although biases in the current photometric approaches can be corrected, in principle,
 by stacking the signals of large ensembles of clusters \citep{Costanzi19},
 large spectroscopic samples, though smaller than the ones suggested here,
 are necessary to calibrate these biases (which change with cluster redshift and possibly cluster mass).
The photometric selection of background objects remains subject to foreground contamination.

Spectroscopic redshifts completely eliminate biases resulting from errors in the inferred redshift distributions.
This approach also eliminates correlations in the signals between tomographic bins originating from sizable errors (random and systematic)
 in photometric redshifts.
Furthermore, spectroscopic samples avoid dilution of the signal that arises from the contamination of background shear samples by cluster galaxies.

Development of spectrotomography will extend the impact of weak lensing from measurement of mass distributions to the determination of cosmological parameters.
Figure \ref{fig:pfs24} shows that constructing deep spectroscopic samples behind even a small sample ($\sim 50$) clusters enables
 a measurement of the actual shape of the angular diameter distance ratio curve.
Because this curve depends on the expansion history of the Universe,
 these samples can provide probes of the cosmological parameters that are independent of other methods \citep{Martinet15}.
In particular, spectrotomography provides a purely geometric test of cosmology, functioning as a completely independent test of cosmography.

\section{Conclusions}

Weak lensing has a broad impact on astrophysics from the study of cluster masses
 \citep{Dahle02, Okabe10, Medezinski10, Umetsu14, vonderLinden14, Hoekstra15, McClintock19} and
 the relationship between the galaxy and dark matter distributions on large scales
 even including the detection of voids \citep{Davies18}.
So far the applications have been limited to the use of photometric data.
For individual clusters the significance of detections has increased steadily from $\sim 4$ \citep{Tyson90}
 to $\sim 15$ \citep{Okabe10, Schrabback18}.
Stacking of large samples has further enhanced the impact of the measurements \citep{McClintock19}.

\citet{Hu02} suggested that
 ultimately spectroscopic tomography could become a powerful astrophysical tool for
 system mass measurements and, ultimately, for sensitive cosmological tests.
Application of spectroscopic tomography requires large, dense complete redshift surveys to significant depth.
Until there have been no such surveys in part because of the time on large telescopes required to make the observations.

Here we report a first spectrotomographic detection.
We use the massive cluster A2029 as a test case.
This cluster ($z = 0.078$) has a mass of $9\times 10^{14} M_\odot$ \citep{Sohn19a}.
The low redshift enables an exploration of the spectrotomographic signal with
 a redshift survey for objects brighter that $r = 20.5$.
The survey we use contain 1517 background objects within $23\arcmin$ of the cluster weak lensing center.

We detect the spectrotomographic signal at a significance of
 $3.9\sigma$ within a $23\arcmin$ radius (and 3.7 $\sigma$ within $13 \arcmin$).
We demonstrate that the signal appears cleanly in the relative distributions of
 cross and tangential ellipticities for sources with spectroscopic redshifts.
We also demonstrate that these sources have identical distributions of $e_{1}$ and $e_{2}$.
Other demonstrations of the robustness of the detection included
 its insensitivity to the exact position of the cluster center and to the redshift binning.

From the physical point of view,
 the spectrotomographic detection shows the expected dependence of the signal
 on the source redshift distribution.
Measurements of this signal with much large samples hold promise for
 a purely geometric cosmological test.

To explore the promise of spectrotomography we simulate observations with PFS on Subaru.
We show that with complete spectroscopic samples to a limiting $i = 22.7$  and $i = 23.7$
 the detections should be in the range $7$ to $12\sigma$.
For the sample to $i = 23.7$, typical surveys would include $\sim 6000$ cluster members
 and $\sim 15000$ background objects.
Thus ancillary benefits of these surveys include foundations
 for the spectroscopic study of both cluster and background galaxy populations
 with unprecedented depth and completeness.

Even for the $i=22.7$ survey case,
 the error bars in the spectroscopic tomography become small enough to support a cosmological probe.
The time require for each cluster observation ($\sim 4$ hours/clusters) implies that
 samples of $>100$ clusters at redshifts similar to A2029 could be observed with
 a reasonable time allocation.
Samples of this size would open an era of spectroscopic tomography.
With multi-object spectrographs on larger telescopes such as GMT,
 these studies could readily be extended to clusters at larger redshift.

\bigskip

\acknowledgments
I.D. acknowledges support from DOE award DE-SC0010010
J.S. is supported by a CfA Fellowship.
M.J.G. acknowledges the Smithsonian Institution for support.
This paper includes data produced by the OIR Telescope Data Center in the Smithsonian Astrophysical Observatory.
This research has made use of NASA`s Astrophysics Data System Bibliographic Services.
Some observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.
Some observations reported here were obtained with the Dark Energy Camera installed on the Blanco Telescope at CTIO, part of NSF's National Optical-Infrared Astronomy Research Laboratory.  The National Optical-Infrared Astronomy Research Laboratory is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation.
Data was extracted from the  CSDC Science Data Archive at NSF's National Optical-Infrared Astronomy Research Laboratory
This research uses the LSST Science Pipelines for shape measurement. Financial support for LSST comes from the National Science Foundation (NSF) through Cooperative Agreement No. 1258333, the Department of Energy (DOE) Office of Science under Contract No. DE-AC02-76SF00515, and private funding raised by the LSST Corporation. The NSF-funded LSST Project Office for construction was established as an operating center under management of the Association of Universities for Research in Astronomy (AURA). The DOE-funded effort to build the LSST camera is managed by the SLAC National Accelerator Laboratory (SLAC).

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


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text:
Lenovo, HP unveil first AMD Fusion laptops
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HP Pavilion dm1 image
The first laptops to use AMD's new Fusion technology were unveiled on Monday in Las Vegas prior to the Consumer Electronics Show, in the form of Lenovo's ThinkPad X120e and HP's Pavilion dm1.
The ultraportables both have 11.6-inch screens, placing them within the size range of the netbook. However, their E-Series 'Zacate' chips, which rival Intel's ubiquitous Atom, give them a significant boost in graphics performance over that found in most netbooks. This is because the processor is what AMD calls an accelerated processing unit (APU), which combines a multicore CPU with a DirectX 11-capable GPU into a single unit.
HP's updated Pavilion dm1, pictured, uses AMD's E-Series 350 APU, which has two cores clocked at 1.6GHz and integrated Radeon HD 6310M graphics.
Photo by: HP
Caption by: David Meyer
HP's new Pavilion dm1 will, according to the manufacturer, provide up to 10 hours of battery life.
Configuration of the ultraportable includes 750GB HDD, while GPS and external Blu-ray are further options. The device has a 1,366x768-pixel display.
The dm1 will go on sale in the US from 9 January, at a starting price of $450 (£289).
Lenovo ThinkPad X120e image
Like HP with the dm1, Lenovo is pitching its ThinkPad X120e at the business user, and is eschewing the 'netbook' moniker for the device.
Lenovo claimed in a statement that the X120e will provide more than six hours of battery life.
Photo by: Lenovo
Lenovo's ThinkPad X120e will go on sale in February, with US prices starting below $400, the company said.
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The flow dynamics in the Gulf of Mexico are dominated by the Loop Current which goes around Cuba (seen on lower right). Eddies spin off the Loop Current at a rate of one every few months. An arrangement of warm core eddies, one detached (left side) and one forming (northwesterly of the Loop Current), is depicted here. Accompanying cold core eddies are also evident. The eddies are delineated by stable and unstable manifolds of various hyperbolic trajectories, and those manifolds are shown here. This is based on a re-creation of the flow field from a specific period in June,1998, using a layered model with satellite data assimilated into the model. One of the most interesting features to note is the greater mixing exhibited around the edges of the cold eddies than the warm eddies. This is evidenced by the more complicated manifold configuration.
Submitted by Picture Gallery editors, not the original authors.