text:
Faculty Home overview
Cambridge Medieval Literature and Culture Seminar 2021-21
About French
Staff in French
Information for Undergraduates overview
Part Ia overview
FRB1: Use of French
FRB1: Use of French overview
FRB1 Programme du trimestre
FRB2: Translation from French
FR1: Introduction to French literature, linguistics, film and thought
Part Ib overview
FRB3: Translation into French
FRAV: French through Audio-Visual Media
FR2: Structure and varieties of French
FR3: Space and Place in Medieval French Literature
FR4: Rethinking the Human: French Literature, Thought and Culture, 1500-1700
FR5: Revolutions in writing, 1700-1900
FR6: Innovation and Upheaval: deformation and reformulation in the 20th and 21st centuries
FRC1: Translation from and into French
FRC2: French: Text and Culture
FR7: Defining the human in medieval French literature and culture
FR8: Wondrous forms in the age of Montaigne
FR9: Reason, experience, and authority: French literature, thought, and history, 1594-1700
FR10: Enlightenment and its limits
FR11: Gender, desire, and power in 19th century French culture
FR12: Ethics and experience: literature, thought, and visual culture of the French-speaking world (1900 to the present)
FR13: The French Language: Variation and Change
FR14: Theatre: theory and practice.
FR15: Voices of Desire
FR16: Colonialism, empire and globalisation: technologies of space in French culture from 1700
Staff Student Liaison
Applications and Funding
PhD Students in French
PhD Students in French overview
French Graduate Research Seminar
What follows is a list of recommended online resources. It is an attempt to provide a cross-section of relevant websites, in the hope that these will be prove useful to students as they pursue their own explorations.
Gateways / Podcasts / French Literature / French Authors / Francophone Literature / Thinkers and Philosophers / French and Francophone history and culture / Cinema / Work Experience
Language Papers
Paper Fr.B1 / Paper Fr.B2 / Paper Fr.B3
Paper Fr.1 / Paper Fr.2 / Paper Fr.3 / Paper Fr.4 / Paper Fr.5 / Paper Fr.6 / Paper Fr.7 / Paper Fr.8 / Paper Fr.9 / Paper Fr.10 / Paper Fr.11 / Paper Fr.13
Gateways/Portals for French students/researchers
Intute Subject Gateway French Studies Portal
The Society for French Studies
Since the legalisation in France of podcasting ("baladodiffusion" for the purist) in January this year, Radio France has far outpaced the BBC in terms of the range of programmes it makes available. You'll find links through to all the major RF stations and the podcasts they offer at:
Link to major RF stations and their podcast
Legally, podcasts are made available until the next episode of a programme is broadcast. While many radio programmes remain accessible for a long period over the internet, the advantage of the podcast (MP3 file) is that it can be downloaded and listened to without an active internet connection, for example when you're travelling to work, walking the dog, cooking or whatever. All you need is an MP3 player and freely available software (typically iTunes, Doppler, Juice) to download the podcasts. You then drag and drop them to your MP3 player, unless of course you simply want to listen on your own computer (Windows Media Player is also an MP3 player). It couldn't be easier, and it's a terrific resource. France Culture, in particular, offers some of its best programmes in this way.
French Literature
Frantext
Erudit's Études littéraires journal
French Authors
gidiana.net
andregide.org
Francophone Literature
Littératures du Maghreb
île en île
Un site culturel et littéraire francophone
French philosophers and thinkers
Jean Khalfa's Fanon Podcast
French & Francophone History & Culture
Society of Dix-Neuviémistes
Equinoxes: a graduate journal of french and francophone studies
Journal of Contemporary French and Francophone Studies
Media Art Net An excellent avant-garde film resource with plenty of clips and articles
Zéro de Conduite Cinéma blog
Blog from film theory legends David Bordwell and Kristin Thompson
UbuWeb: a completely independent resource dedicated to all strains of the avant-garde, ethnopoetics, and outsider arts
Radical Philosophy journal of socialist and feminist philosophy
Bibliothèque du film
Cadrage.net 1ère revue en ligne universitaire française de cinéma
Cahiers du Cinéma.com
Film-Philosophy.com
Africultures Le Site et la Revue de Référence des Cultures Afraicaines
le Film Francais.com
Forum des Images
Departmental Film Collection
Tout sur le cinéma
Film Philosophy
Film Magazine
Objectif Cinema
Screen - journal of academic film and television studies
Zéro de Consuite cinéma blog
Yale Film Studies Film Analysis Web Site
Télédoc excellent site sur le cinéma, fiches pédagogiques sur films et documentaires (en particulier "plans rapprochés et anciens "dossiers"), liens utiles etc.
Arrêt sur images excellent site sur l'analyse des médias
Jenny Chamarette's site dedicated to Cléo de 5 è 7
CVs in French
Paper Fr B1 Use of French
Programme du trimestre (Grammar)
dossier Francophonie (Language Centre)
dossier Mai 68 (Language Centre)
Practice Use of French papers elaborated by students - Example 1 and Example 2
lepointdufle.net an excellent site for French grammar and more
"des banlieues"
Études-littéraires.com (explore section "langue" in particular). Great for grammar, rhetorical terms, stylistics
Le Conseil International d'Études Francophones recommended texts
Le français par les peintres
The Académie Française' Questions de Langue
Centre Images Initiation au vocabulaire de l'analyse filmique
Mondesfrancophone.com's Excellent site on Francophone writers/intellectuals
Radio France International (incorporating some excellent pedagogical resources)
TV5 Monde's audiocasts
Linguee's combined dictionary and search engine- a great resource for contextual translations
Recommended books, films and links (useful for Cambridge applicants and students!)
French by Repetition. Great website for key expressions - created by a former MML student!
Paper Fr B2 Translation of French and Oral B
Gustave Flaubert — Madame Bovary (Sylvia Huot)
Gustave Flaubert — Madame Bovary II (Sylvia Huot)
André Gide - Les Faux Monnayeurs (Sylvia Huot)
Madame de Lafayette - La Princesse de Clèves (1678) (Sylvia Huot)
De l'expérience - Michel de Montaigne (Sylvia Huot)
François Rabelais - Pantagruel (Le Quart Livre) (Sylvia Huot)
Paper Fr B3 Translation into French and French though audio-visual media
Please also consult the FR11 section on cinema for more film reviews in French
Talking it Over, 1992 - Julian Barnes (Christophe Gagne)
Travels with my Aunt - Graham Greene
The Golden Notebook, 1962 - Doris Lessing
A Year in Provence - Peter Mayle (Michèle Hagard)
Passage from Mister God this is Anna (Student example work: Camilla and Annie)
Captain Corelli's Mandolin (Student example work: Natalie S. Higgins, Sarah Nye Jen Wainwright)
Guy Browning – How to...lie in (Student example work: Paul Moyses and Latifa Sadoc)
The Importance of Being Earnest and its translation (Student example work: George Walkden, Natasha Mann, Alastair Shaw )
Alice in Wonderland, its translation and commentary (Student example work: George Austin-Cliff, Polly Dickson)
The poetry and musings of Stanford Fraser
Jenny Chamarette's site dedicated to Cléo de 5 à 7
Mock Exam and Corrections
Online Videos (Language Centre)
france5.fr
INA clips, (analyse de l'image section, Jalons de l'histoire), a brilliant website to work on your FRAV skills and learn more about French History
Teledoc: a brilliant website to work on your film analysis skills (dossiers pédagogiques, télé è la loupe)
Études-littéraires.com
A selection of five inspiring TED.com talks in French
Scheduled Paper Resources
Paper Fr 1 Introduction to the structures and varieties of modern French
Languefrancaise
Introduction à la linguistique française
SIL International French/English Dictionary of Linguistic Terms
Grammar and Structures
Regional variation within France
A general introduction to French linguistics
Phonetics (good for practising sound recognition)
Délégation à la langue française (neologisms, borrowings in the 'vocabulaire et terminologie' section)
Phonetics (regional variation within France)
French in the world
On creoles
Paper Fr 2 French literary texts: an introduction
Études-littéraires.com a great website to learn more about French literature
Cléo de 5 à 7
muse.jhu.ed on Cleo and its context
From Feminine Masquerade to Flâneuse: Agnès Varda's Cléo in the City Janice Mouton. Cinema Journal, Vol. 40, No. 2 (Winter, 2001), pp. 3-16
Reflections in a Broken Mirror: Varda's Cléo de 5 à 7 Roy Jay Nelson. The French Review, Vol. 56, No. 5 (Apr., 1983), pp. 735-743
Phèdre
Medea, Poison, and the Epistemology of Error in Phèdre Amy Wygant. The Modern Language Review, Vol. 95, No. 1 (Jan., 2000), pp. 62-71
Guérin's Painting of Phèdre and the Post-Revolutionary Revival of Racine James Henry Rubin. The Art Bulletin, Vol. 59, No. 4 (Dec., 1977), pp. 601-618
Phèdre et les dieux Carlo François. The French Review, Vol. 35, No. 3 (Jan., 1962), pp. 269-278
Politics and Passion in Phèdre C. E. Nelson. The French Review, Vol. 39, No. 1 (Oct., 1965), pp. 22-3
Double Vision in Racine's Phèdre Thomas J. Braga. The French Review, Vol. 64, No. 2 (Dec., 1990), pp. 289-298
Une Aventure théâtrale en classe: Phèdre Claude Abraham. The French Review, Vol. 60, No. 2 (Dec., 1986), pp. 209-215
The "Labyrinthe": A Metaphor of Dramatic Action in "Phedre" Pierre Han. South Atlantic Bulletin, Vol. 34, No. 4 (Nov., 1969), pp. 15-17
Phèdre, ou la liberté dans l'acte héroïque Michelle Coquillat. The French Review, Vol. 47, No. 5 (Apr., 1974), pp. 857-864
The Space of Phedre Anne Ubersfeld, Mya Weinberger, J. Cairncross. Poetics Today, Vol. 2, No. 3, Drama, Theater, Performance: A Semiotic Perspective (Spring, 1981), pp. 201-210
Deracination: Phedre's Monstrous Pedagogy Krystian Czerniecki. MLN, Vol. 103, No. 5, Comparative Literature (Dec., 1988), pp. 1012-1030
Phedre: Le Monde reel et les mondes imaginaires dans le theatre de Racine Marie-Rose Carré. PMLA, Vol. 81, No. 5 (Oct., 1966), pp. 369-376
Narcisse mortifié et mortifère: le regard chez Racine Renée Morel. The French Review, Vol. 64, No. 6 (May, 1991), pp. 921-933
Sappho, c'est moi, selon Racine: Coming of Age in Neo-Classical Theater Joan Dejean. Yale French Studies, No. 76, Autour de Racine: Studies in Intertextuality (1989), pp. 3-20
Les Faux Miroirs: The Good Woman/Bad Woman Dichotomy in Racine's Tragedies Véronique Desnain. The Modern Language Review, Vol. 96, No. 1 (Jan., 2001), pp. 38-46
The Theatricality of Discourse in Racinian Tragedy Henry Phillips. The Modern Language Review, Vol. 84, No. 1 (Jan., 1989), pp. 37-50
Thérèse Raquin
Thérèse Raquin et Manet: harmonie en gris Jurate D. Kaminskas. The French Review, Vol. 57, No. 3 (Feb., 1984), pp. 309-319
The Mirror, The Window, and The Eye in Zola's Fiction Philip Walker. Yale French Studies, No. 42, Zola (1969), pp. 52-67
Aspects of the Psychology of Love in the Heptameron Mary J. Baker. The Sixteenth Century Journal, Vol. 19, No. 1 (Spring, 1988), pp. 81-87
Gendered Virtue, Vernacular Theology, and the Nature of Authority in the Heptameron Carol Thysell. The Sixteenth Century Journal, Vol. 29, No. 1 (Spring, 1998), pp. 39-53
Platonism - Myth or Reality in the Heptameron? Robert W. Bernard. The Sixteenth Century Journal, Vol. 5, No. 1 (Apr., 1974), pp. 3-14
Feminine Authority in the "Heptaméron": A Reading of Oysille Paula Sommers. Modern Language Studies, Vol. 13, No. 2 (Spring, 1983), pp. 52-59
Fictional Truth and the Prologue of the "Heptameron" Sylvie L. F. Richards. Rocky Mountain Review of Language and Literature, Vol. 48, No. 1 (1994), pp. 61-76
Magdalen's Skull: Allegory and Iconography in Heptameron 32 Francois Rigolot. Renaissance Quarterly, Vol. 47, No. 1 (Spring, 1994), pp. 57-73
Marguerite de Navarre's Heptaméron: The Case for the Cornice Paula Sommers. The French Review, Vol. 57, No. 6 (May, 1984), pp. 786-793
Vision and Voyeurism in the "Heptaméron: Re-Reading the 43rd Novella" Paula Sommers. Modern Language Studies, Vol. 22, No. 1 (Winter, 1992), pp. 88-95
Realism and Closure in the "Heptameron": Marguerite de Navarre and Boccaccio John D. Bernard. The Modern Language Review, Vol. 84, No. 2 (Apr., 1989), pp. 305-318
Death's Desire: Sensuality and Spirituality in Marguerite de Navarre's "Heptaméron" Richard Regosin. MLN, Vol. 116, No. 4, French Issue (Sep., 2001), pp. 770-794
Didacticism and the Heptaméron: The Misinterpretation of the Tenth Tale as an Exemplum M. J. Baker. The French Review. Special Issue, No. 3, Medieval and Renaissance Studies (Autumn, 1971), pp. 84-90
The Heptaméron and the Foundation of Critical Narrative John D. Lyons. Yale French Studies, No. 70, Images of Power Medieval History/Discourse/Literature (1986), pp. 150-163
Les Lettres persanes
La Pensée et l'action dans les Lettres persanes Bernard Picard. The French Review, Vol. 42, No. 6 (May, 1969), pp. 857-864
The Would-Be Invisible Chain in Les Lettres persanes R. L. Frautschi. The French Review, Vol. 40, No. 5 (Apr., 1967), pp. 604-612
Montesquieu the Novelist and Some Imitations of the "Lettres Persanes" F. C. Green. The Modern Language Review, Vol. 20, No. 1 (Jan., 1925), pp. 32-42
Libertarian Demography: Montesquieu's Essay on Depopulation in the Lettres Persanes David B. Young. Journal of the History of Ideas, Vol. 36, No. 4 (Oct. - Dec., 1975), pp. 669-682
Rereadings in Orientalism: Oriental Inventions and Inventions of the Orient in Montesquieu's "Lettres persanes" Lisa Lowe. Cultural Critique, No. 15 (Spring, 1990), pp. 115-143
The Place and Sense of the "Outsider:" Structuralism and the Lettres Persanes Suzanne Gearhart. MLN, Vol. 92, No. 4, French Issue (May, 1977), pp. 724-748
Paper Fr 3 French literature, thought, and history, before 1300
Andreea Weisl-Shaw's website for students of Fr 3
Paper Fr 4 Occitan Literature, Thought, and History, before 1356
Paper Fr 5 French literature, thought, and history, from 1300 to 1510
The Société Française d'Etude du Seizième Siècle
Epistemon
Eglal Henein, Deux visages de L'Astrée, critical edition of the first and second volume of Honoré d'Urfé's L'Astrée, 2005, 2007, 2010
Eighteenth-century resources
From the University of Portsmouth: excellent overviews on some of the key historical aspects of the period you are studying
Paper Fr 9 French Literature, Thought and History from 1789 to 1898
Dix-Neuf, the Society of Dix-Neuviémistes
J.-K. Huysmans (1848-1907)
L'Histoire de France par l'image
ClicNet: Littérature francophone virtuelle du XIXe siècle
Gallica - Images et textes du XIXe siècle (click on Découverte, then XIXe to access a list of C19 themes)
Brown University Library Center for Digital Initiatives (on C19 Paris)
19th-Century French Studies Resources
Le XIXème siècle (1815-1914)
Balzac, La Comédie Humaine en ligne
Paper Fr 10 French Literature, Visual Culture, Thought and History from 1890 to 1958
Le site officiel Guillaume Apollinaire
FR10: French Literature, History and Thought since 1890
pennsound: an excellent site for French poetry
Paper Fr 11: Literature, Visual Culture, Thought and History in the French-speaking World Since 1945
La Cinémathèque Bibliothèque du film
Francophone Internet Resources @ Lehman College, CUNY
Collectif Littéerature
Jean-Michel Maulpoix
Littèrature contemporaine
La Revue des Ressources
Paper Fr 13 The French Language: Variation and Change
Summer Institute of Linguists Languages in Contact Website
Codeswitching Bibliography Database
Foundation for Endangered Languages
Podcast of Professor Peter Trudgill's talk "Languages in Contact and Isolation: Mature Phenomena and Societies of Intimates"
Regional French and Dialectology
Accents de France
Jerriais (1)
Guernesiais
Norman dictionaries
The Anglo-Norman Correspondence Corpus
Anglo-Norman On-line hub
Continental Norman
Sercquais
Rapport Barère
Rapport Grégoire
Seselwa
History of the French Language
Database of French texts
Histoire de la langue française
Language Endangerment
UNESCO Atlas of the World's Languages in Danger
Podcast of Christopher Moseley's talk "Mapping Linguistic Endangerment: The UNESCO Atlas of the World's Languages in Danger"
Elly Walters wins 2020 Outstanding Student Contribution to Education Award from CCTL
Congratulations to Elly Walters, who was just given an OSCEA award by the Cambridge Centre for Teaching and Learning for Inclusive Practice.
Recent alumna Ellen Weaver publishes article in Columbia Journal of History
Congratulations to Ellen Weaver (MMLL 2019) who has just had an article entitled, 'Representations of the Bumidom: Reembodied Histories in Jessica Oublié and Marie-Ange Rousseau's Péyi An Nou', published in the Columbia History Journal.


text:
Dagger Records
Jimi Hendrix Photos
Jimi Hendrix Videos
Concert Broadcasts
Experience Hendrix Tour
Jimi Hendrix Encyclopedia
Did you see Jimi Hendrix in concert? Did you meet Jimi Hendrix or have the opportunity to interview him or have some other unique, first-person encounter with Jimi Hendrix? If so, Experience Hendrix wants to hear from you.
Nov Dec Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Jan Feb Mar Apr May Jun Jul Aug Sep
01/1967 02/1967 03/1967 04/1967 07/1967 01/1968 02/1968 03/1968 04/1968 05/1968 06/1968 08/1968 09/1968 11/1968 03/1969 06/1969 07/1969 11/1969 12/1969 01/1970 04/1970
02/1967 03/1967 01/1968 03/1968 04/1968 05/1968 06/1968 07/1968 08/1968 09/1968 10/1968 11/1968 12/1968 01/1969 02/1968 03/1968 05/1968 06/1968 07/1968 11/1969 03/1970 04/1970
04/1967 03/1969 12/1969 01/1970 02/1970
01/1967 02/1967 03/1967 04/1967 01/1968 02/1968 03/1968 04/1968 05/1968 07/1968 09/1968 10/1968 11/1968 01/1969 02/1969 03/1969 04/1969 05/1969 12/1969 01/1970 02/1970 03/1970 08/1970
01/1967 02/1967 03/1967 04/1967 01/1968 02/1968 03/1968 05/1968 10/1968 03/1969 04/1969 11/1969 03/1970
03/1967 01/1968 02/1968 04/1968 08/1968 09/1968 01/1968 03/1969 05/1969 06/1969 07/1969 11/1969 02/1970 03/1970 04/1970 05/1970 06/1970 08/1970
07/1967 08/1967 09/1967 10/1967 01/1968 02/1968 04/1968 05/1968 06/1968 07/1968 08/1968 10/1968 12/1968 01/1969 02/1969 03/1969 04/1969 05/1969 06/1969 08/1969 11/1969 12/1969 01/1970 02/1970 03/1970 05/1970 06/1970 07/1970 08/1970
01/1967 02/1967 03/1967 04/1967 01/1968 02/1968 03/1968 04/1968 05/1968 06/1968 07/1968 08/1968 09/1968 10/1968 11/1968 12/1968 01/1969 04/1969 05/1969 06/1969 01/1970 02/1970 03/1970 05/1970 06/1970 07/1970 08/1970
Live 1967 United Kingdom Recording the experience Interviews London live performance The Jimi Hendrix Experience interview Soft Machine Personal Jimi Hendrix February Events March April Media Band January
The Jimi Hendrix Experience performance at the Astoria in Oldham, Lancashire.
1967 Astoria January January 22 Lancashire Live live performance Oldham United Kingdom
Back at the Record Plant, rough mixes of "Sky Blues Today" and "Izabella" were prepared but later scrapped in favor of new ones.
1970 Izabella January 22 Recording rough mixes Sky Blues Today the Record Plant
Jimi Hendrix Newsletter
LEGACY and the "L Legacy" logo are registered trademarks of Sony Music Entertainment.
I Am Experienced
© 1996-2021 Experience Hendrix, L.L.C. All Rights Reserved.
"JIMI HENDRIX" and related logos are trademarks of Experience Hendrix, L.L.C.

redpajama_set_name: RedPajamaCommonCrawl


After a huge success in Hillsboro, Flyhomes' PDX Team is headed to Southeast Portland for the next stop on the neighborhood tour!
Come join us at TABORSPACE in the Library on Saturday, February 9th from 1-3pm. Learn about housing market trends in your neighborhood and meet the team that can help you buy and sell with a brand new approach in the new year.
Snacks and refreshments on us.


text:
Jewish and Russian Revolutionaries Exiled to Siberia (1901-1917)
Author: Desind, Philip
This scholarly yet highly readable work offers two unique autobiographical perspectives on the early days of the Russian revolution, heretofore unavailable to the English-speaking world. The first perspective, an individual Jewish revolutionary from Byelorussia politically exiled to Siberia, is Desind's contemporary translation from the Yiddish of a prize-winning autobiography by Israel Pressman written in the 1940's, recalling the first decade of this century. The second perspective is that of the Izmailovich sisters, daughters of a high ranking military family. Their story represents not only a divergent approach to the revolution, but also the significant role played by women in fighting Russian autocracy. The material is based on Russian documents and supplemented by several English sources. The two individual accounts are explicated and impressively enriched by pertinent notes and essays which provide the historical and sociological framework for the lives portrayed in the two dramas. Includes rare photographs.
"Desind's book is an attempt to combine a primary source in translation and a historical narrative under a single cover, supplemented by supporting materials in the notes. The volume is therefore of particular value for readers interested in Russian revolutionary history who lack an adequate command of the Russian language to allow them to use primary sources. . . . Desind's translation of the autobiography of Israel Pressman . . . is the only English translation of the work and thus introduces a valuable new source depicting the emergence of a radical from the traditional Jewish milieu. . . . The reader is also indebted to Desind for his thoughtful and accurate translation and his capable editorial efforts. He has been able to obtain a number of new and interesting photographs from private collections and compiled a useful bibliography of works in English. . . . will be appreciated especially by nonspecialist interested in Jewish radicalism and Russian revolutionary history in general." - The Russian Review
Desind has made a contribution to the literature on the revolutionary movement. A participant's memoir is the voice of authenticity, complementing historical monographs. The book is filled with ample footnotes and many brief commentaries on aspects of Russian-Jewish life and history." - Shofar
Other Jewish Studies Books
2018 - The Spiritual Disorder of the Jews and the Need for a Zionist Renaissance: A History of the Ongoing Debate
1993 - Origins of the British Israelites: The Lost Tribes
1998 - Theologies of War and Peace Among Jews, Christians, and Muslims
>> See all our Jewish Studies books


text:
Ясен (Fraxinus) — рід листопадних дерев родини маслинових (Oleaceae).

село Ясень, Рожнятівський район Івано-Франківської області

Населені пункти та їхні частини

 Ясень — місто в Жарському повіті Любуського воєводства
 Ясень — гміна в Жарському повіті Любуського воєводства
 Ясень — село в гміні Тлухово Ліпновського повіту Куявсько-Поморського воєводства
 Ясень — село в гміні Осьякув Велюнського повіту Лодзинського воєводства
 Ясень — село в гміні Ґлухув Скерневицького повіту Лодзинського воєводства
 Ясень — село в гміні Любохня Томашовського повіту Лодзинського воєводства
 Ясень — село в гміні Роґув Бжезінського повіту Лодзинського воєводства
 Ясень — село в гміні Бжесько Бжеського повіту Малопольського воєводства
 Ясень — село в гміні Репкі Соколовського повіту Мазовецького воєводства
 Ясень — село в гміні Чарна Домбрувка Битівського повіту Поморського воєводства
 Ясень — село в гміні Сташув Сташовського повіту Свентокшиського воєводства
 Ясень — село в гміні Хмельник Келецького повіту Свентокшиського воєводства
 Ясень — село в гміні Лопушно Келецького повіту Свентокшиського воєводства
 Ясень — село в гміні Чемпінь Косцянського повіту Великопольського воєводства
 Ясень — частина міста Устрики-Долішні в Бещадському повіті Підкарпатського воєводства
 Ясень — частина міста Гданська в Поморському воєводстві
 Ясень — колонія в гміні Кобеле-Вельке Радомщанського повіту Лодзинського воєводства

Примітки

redpajama_set_name: RedPajamaWikipedia


Set up an existing model comp to specified values.
Set up list of dependencies for this component.
Print a detailed description of this model component and all its fields.
Print a one line description of the object (type and name).
Tag this components and all its dependencies recursively.
Recalculate dependency list and re-resolve IDREF nodes.
Whether the component has a tag.
Retrieve the value of this component (if a set or parameter).
Set the value for this component.
Move this model component up in the model tree.
Duplicate the object: shallow copy.
Duplicate the object: deep copy.
Set the tag to false for all models: using global_list.
Recursively set the tag to false for all models.
Recursively write name of all tagged components.
Write definition of all tagged components to file, using global_list.
A tree of specifications (which includes :=, within, default, >=).
The model this component belongs to.
A pointer to an AmplModel structure for components of type MODEL.
List of all entities that this model component depends on.
Components can be tagged by the tagDependencies method which sets this tag for this components and everything that it depends on (i.e.
For sets and parameters, this points to an object that gives the values and further specific information (Set for sets).
Find dependencies for this component.
Global list of all defined ModelComps.
Object to represent a component of an AMPL/SML model/block.
It usually represents one line of AMPL/SML which is a definition of a variable/parameter/set/constraint/objective/block.
Construct a model component given its name, id, indexing and attribute sections.
References count, global_list, indexing, PRINT_LOG, GlobalVariables::prtLvl, and setUpDependencies().
Default constructor: just sets all fields to -1/NULL/false.
Create a shallow copy of the object: only the top level object is copied, pointers below are reused.
References attributes, count, dependencies, indexing, model, ModelComp(), other, tag, and type.
Referenced by StochModel::expandToFlatModel(), and write_ampl_for_submodel_().
Create a deep-copy of the ModelComp object.
The tree of attributes and indexing expressions is recreated using entirely new objects.
References attributes, count, SyntaxNodeIx::deep_copy(), SyntaxNode::deep_copy(), dependencies, indexing, model, ModelComp(), other, tag, and type.
References attributes, count, dependencies, indexing, model, AmplModel::name, nameTypes, SyntaxNodeIx::splitExpression(), tag, CompDescr::toString(), type, and value.
References dependencies, SyntaxNode::findIDREF(), and LogMC.
Referenced by StochModel::expandStagesOfComp(), and StochModel::expandToFlatModel().
Write out a list of all model components that have the tag set: write every component how it would appear in the global model file.
modified_write should be called within the model writing process: it depends on addIndex/l_addIndex, i.e. some indexing expressions (and subbmodel names) should be added to entity names depending on where in the model it is called.
Referenced by expandSet(), and StochModel::expandStagesOfComp().
Queue the ModelComp to be moved up by 'level' levels in the model tree: Just removing the component from the current model and adding it to a parent is dangerous, since ModelComp::moveUp is typically called from within a (nested) loop over all ModelComps (->comps) in the AmplModels removing/adding items to list<ModelComp*> comps while there is an iterator running over it will invalidate that iterator.
References attributes, CHANGE_ADD, CHANGE_REM, AmplModel::changes, SyntaxNode::findIDREF(), SyntaxNodeIx::getDummyVarExpr(), SyntaxNodeIx::getNComp(), indexing, AmplModel::ix, model, AmplModel::parent, SyntaxNode::push_front(), and SyntaxNodeIDREF::ref.
In the process of building the AmplModel tree from the StochModelTree some of the IDREF dependency nodes still point to the StochModelComp nodes from the StochModel tree (or the intermediate tree).
This routine makes sure that IDREF nodes are resolved with respect to the correct ModelComp and rebuilds the dependency lists.
References attributes, AmplModel::comps, dependencies, SyntaxNode::findIDREF(), id, indexing, model, PRINT_INFO, GlobalVariables::prtLvl, and SyntaxNodeIDREF::ref.
Set a model component to a given name, id, indexing and attribute sections.
References attributes, count, global_list, indexing, setUpDependencies(), tag, tt_count, and type.
Set up the list of dependencies for this component.
References attributes, dependencies, findDependencies(), indexing, LogMC, and SyntaxNode::print().
Referenced by AmplModel::addComp(), ModelComp(), and setTo().
Recursively set tag=true for this model component and all components that it depends on (i.e. everything listed in its dependency list).
Set tag=false for all model components.
Referenced by expandSet(), StochModel::expandStagesOfComp(), untagAll(), and write_ampl_for_submodel().
Recursively set tag=false for all model components.
start The AmplModel where to start the recursion.
References AmplModel::comps, TMODEL, and untagAll().
Recursively write out a list of all model components that have the tag set.
References AmplModel::comps, AmplModel::name, and TMODEL.
Referenced by StochModelComp::clone(), clone(), deep_copy(), dump(), AmplModel::find_var_ref_in_context(), modified_write(), moveUp(), print_entry(), reassignDependencies(), setTo(), setUpDependencies(), and StochModelComp::transcribeToModelComp().
Referenced by StochModelComp::clone(), clone(), deep_copy(), dump(), ModelComp(), and setTo().
This lists all model components used in the definition of this component.
Referenced by StochModelComp::clone(), clone(), deep_copy(), dump(), findDependencies(), reassignDependencies(), setUpDependencies(), and tagDependencies().
Referenced by ModelComp(), modifiedWriteAllTagged(), setTo(), and untagAll().
Referenced by CompDescrParam::CompDescrParam(), AmplModel::createExpandedModel(), end_smodel(), AmplModel::find_var_ref_in_context(), getGlobalName(), getGlobalNameNew(), labelToSetElement(), modified_write(), print_entry(), print_SyntaxNodesymb(), process_model(), SyntaxNodeIDREF::put(), reassignDependencies(), AmplModel::removeComp(), StochModelComp::transcribeToModelComp(), and write_ampl_for_submodel_().
Referenced by StochModel::_transcribeComponents(), AmplModel::addDummyObjective(), buildPathProbTerm(), StochModelComp::clone(), clone(), CompDescrParam::CompDescrParam(), deep_copy(), dump(), StochModel::expandToFlatModel(), AmplModel::find_var_ref_in_context(), getGlobalNameNew(), ModelComp(), modified_write(), moveUp(), print_entry(), process_model(), reassignDependencies(), setTo(), setUpDependencies(), StochModelComp::transcribeToModelComp(), write_ampl_for_submodel_(), and AmplModel::writeTaggedComponents().
Referenced by AmplModel::addComp(), StochModelComp::clone(), clone(), deep_copy(), dump(), getGlobalName(), getGlobalNameNew(), modified_write(), moveUp(), reassignDependencies(), StochModelComp::transcribeToModelComp(), and write_ampl_for_submodel_().
Referenced by dump(), AmplModel::find_var_ref_in_context(), and printBrief().
Better implemented as a subclass of ModelComp.
Referenced by StochModel::_transcribeComponents(), AmplModel::addComp(), AmplModel::addDummyObjective(), begin_model(), begin_smodel(), StochModelComp::clone(), clone(), AmplModel::createExpandedModel(), deep_copy(), AmplModel::dump(), end_smodel(), StochModel::expandToFlatModel(), fill_model_list_(), print_model(), process_model(), AmplModel::setGlobalNameRecursive(), write_ampl_for_submodel_(), and AmplModel::writeTaggedComponents().
Referenced by StochModelComp::clone(), clone(), deep_copy(), dump(), isTagged(), setTo(), and tagDependencies().
Referenced by StochModel::_transcribeComponents(), AmplModel::addComp(), AmplModel::addDummyObjective(), StochModelComp::clone(), clone(), AmplModel::createExpandedModel(), deep_copy(), dump(), AmplModel::dump(), StochModel::expandStagesOfComp(), StochModel::expandToFlatModel(), fill_model_list_(), AmplModel::find_var_ref_in_context(), modified_write(), print_entries(), print_model(), printBrief(), process_model(), AmplModel::removeComp(), AmplModel::setGlobalNameRecursive(), setTo(), StochModelComp::transcribeToModelComp(), write_ampl_for_submodel_(), and AmplModel::writeTaggedComponents().
Referenced by dump(), getValue(), and setValue().


A municipal billing and collection solution designed for local government utility operations that expedites bill processing, cash collection and control.
The CityShare® Revenue Management suite is a complete and fully integrated billing and collection solution designed specifically for local government entities. The suite enables faster and more accurate bill processing, streamlines cash collection and improves service levels for residents. It has comprehensive functionality that automates tasks to speed your processing, improve revenue collections and provide a real value in total cost of ownership. All applications utilize a consolidated database with a secure user login with access control, departmental reporting and electronic signoffs. The applications provide workflow controls to send notifications or emails to users based on predefined workflow events. Together the applications provide everything you need to deliver a more effective governmental accounting solution.


text:
Photo by Tom Swinnen on Pexels.com
Blog / Press Release
National Nonprofit Opens Affiliate Program in Seattle
Giving Grove orchards provide free fruits, nuts and berries for neighborhoods facing food insecurity
Seattle, WA — The Giving Grove, a national nonprofit serving food insecure communities, announces today it will expand into Seattle in partnership with Tilth Alliance, a Seattle nonprofit that works in community with Washington farmers, gardeners and eaters to build a sustainable, healthy and equitable food future.
Since its launch in 2013, The Giving Grove network has planted 304 orchards across the nation that transform unused and vacant land into safe green spaces that provide free holistically-grown fruits, nuts, and berries. Giving Grove's mission is to provide healthy calories, strengthen community, and improve the environment through a nationwide network of sustainable little orchards that dramatically increase access to healthy foods.
"We are excited to partner with Giving Grove to bring resources and expertise in support of the establishment of Community Orchards, which we view as a vital component to a healthy and equitable food future in Seattle," said Melissa Spear, Tilth Alliance Executive Director. "Establishing these new orchards as a community food resource will result in fresh, culturally relevant, and accessible food for decades to come and provide increased access to public green spaces stewarded and enjoyed by local communities."
After finding success with its model in Kansas City, The Giving Grove began expanding to other cities with high food insecurity rates, launching affiliate programs in St. Louis and Omaha in 2017 and in Memphis, Louisville, rural Kansas, and Cincinnati in 2020. This month The Giving Grove has announced its expansion into Dallas, Atlanta, and Seattle. The Giving Grove's expansion plans include launching affiliates in 11 more U.S. cities by 2025.
"We now have Giving Grove programs from the East to the West coast. With each new affiliate added, we expand the diversity of programming, growing smarter and nimbler as a network. Volunteer orchard stewards caring for a single orchard in one city will have the lessons and experience of the 300 that came before," said Giving Grove Chief Replication Officer Ashley Williamson.
The typical Giving Grove orchard will produce more than 9,800 servings of holistically-grown, free, healthy foods worth more than $8,200 each year. With a 50-60+ year lifespan, each orchard will produce over its lifetime more than 212,000 servings of food for people in need while sequestering carbon, reducing stormwater runoff, and providing urban tree canopy.
Giving Grove's vision is thousands of little orchards in food insecure urban neighborhoods across the nation, creating a local food production system that feeds people for decades. Learn more at www.givinggrove.org.
Tilth Alliance works in community with Washington farmers, gardeners and eaters to build a sustainable, healthy and equitable food future. Learn more at www.tilthalliance.org


Relax to these 10 pristine original Field Recordings from Crypticon Records. Collected after a mountain forest rainy season, these creek sounds will immerse your soul into the very spots of these places, as single track stereo recordings of pure nature.
The Doctor is back in session! Ease your modern day pains with a modern day recording collection of California's finest watery creek sounds. These Field Recordings were captured at a very high quality and minimally processed to bring you direct pristine nature environment tracks available for you here. The microphone was strategically, and in cases, precariously, perched into the brooks, streams and tributaries of the Santa Cruz Mountains during the Winter/Spring season of 2016.
WHITE NOISE IS PEACE AND QUIET MASKED!
Use the powers of Dr. White's Noise to create a foundation of sound to sleep in noisy environments like rooms with snorers, babies, street noise, creaking walls, hobgoblin sounds and other spooky bumping sounds in the night. Use in dorms or when studying to create a sound foundation that you can concentrate from. Nothing is worse than trying to concentrate only to be distracted by sounds unbecoming that in an of themselves are quiet (chewing gum/clicking pencils/flipping paper etc) but can be distracting in low general ambience environments. Bringing up the level of ambience via these sound tracks is a perfect way to concentrate and keep your brain from lingering off into the silence to try to find the sound that shreds the moment, due to the nature of silence and the sound effect.. Now, the low-impact sounds will be drowned out and essentially cancelled due to living under the tones of these type of album sound environments.
White Noise is a science - and Dr. White has his Masters in Field Recording and Sound Mastering from Crypticon Records.
* It is advisable to use the restroom before falling asleep to this album! Side-effects are wetting the bed and/or couch, but definitely yourself. We are not liable to replace linens or clothing. Please remember you are not actually drowning in a river if you wake up while this is playing and immediately panic. If the sounds of water last longer than the prescribed 10 half-hour recordings (5 hours) please check that there is not a flood outside and/or the shower is not running and/or shuffle is not selected.
It is not advisable to take Dramamine while listening to this album as you will not actually get sick from the water noise. Your balance will be maintained due to the almost-certainty that you are listening to this on land. However, listening to his while in a boat and/or airplane is untested and we eagerly await your trial-by-guinea pig adventure and subsequent comments. We will use your input to better craft this very warning letter. We appreciate your commitment. Doctor White assumes no liability if this album is misused to torture those in dense urban environments with what they cannot have in a vertically integrated city and they come back and hobble you for it. Please use to induce peace where necessary. This very album may be used in riot control in conjunction with appropriate crowd control psychotropic mind sprays. This album will not keep you hydrated via osmosis or telekinetic water drawing powers - please drink a half-gallon of water a day to maintain your humanity. This album will not induce rust, but it would be deemed a form of torture to continually play this album for a robot without rust inhibition coatings - see Steampunk for brass construction of your robots by the way (the Doctor is an avid roboticist between midnight and 3am).
Thank you for reading this far, please support us for archiving the audio environments of this planet in this era.


This 29"x29" Flour Sack Towel is printed with a vintage Rooster print. It is beautifully tied with twine and a cute vintage hang tag. This towel is printed and assembled in the USA by American workers. The towel is 100% cotton from Pakistan.


text:
void * bufferFile(const char * file, int * sz);
unsigned int getFileSize(FILE* fp);

extern far_t hArc;

#endif

redpajama_set_name: RedPajamaGithub


apparently it's November, I coulda sworn it was October last month? but anways it's here and as usual on top form I'm late. However I'm also in Prague and there's every chance I'll have something to blog about every day if I get the chance.
We left our house about 11am this morning, 12 hours later we're sat exhausted in our Prague hotel room (Miss Sophies') watching a 90's Music channel whilst eating novelty foodstuff such as Duff beer and paprika flavoured pretezel sticks.
Everything was going fine for most part, we got a taxi to the train station, a train to the airport, checked in painlessly, then queued for about 30 minutes for security before relaxing in Manchester airport's Terminal 1 which we've not been in before, it's a lot better than either 2 or 3 which ever one serves First Choice and Easy Jet! there's actually a choice of bars/restaurants for a start – rather than one of each, also actual airport shopping if that's your thing. Quite impressed.
Then at 2pm we tootled off to our departure gate as requested, where we were promptly told that the plane we were supposed to be departing on in 25 minutes time had a fault that had to be located and repaired by engineers and that we could leave the gate area but to be back in half an hour. Long story short we ended up landing over an hour late, after a more than crappy flight. Stroppy air hostesses (thanks Jet 2), drunk stag groups, and there being no room in the over head lockers as the cabin crew use it as overspill not to mention the couple next to us who managed to have a blazing row just as the plane was coming in to landing that went on until well after disembarkation!
Being 1.5 hours late might not sound that big a deal but try finding a restaurant with a spare table at 8pm on a friday night in a city that apparently does not embrace the "stool at the bar, have a drink while you wait" culture that we've grown accustomed to at home! By some sheer fluke (after being turned away from about 7 restaurants) one had the foresight to seat smaller groups of people on larger tables, we shared with a German family which we had no problem with, in Pivovarský dům, a very popular microbrewery very close to our hotel (which we'd visited previously).
Here I took advantage of the beer sampler option – 8 miniture 'pint' glasses holding 0.1L each of the following beers: traditional Czech pale lager, traditional Czech dark lager, coffee beer, sour cherry beer, wheat beer, Monthly special beer (blueberry), Nettle beer and banana beer!


Igloos are not just for Christmas! Dust off your snow boots, leave your poles at the door and chill out in Tooting's toastiest igloos at The Castle on the High Street. The Warner Edwards Igloos are the ultimate winter retreat – fully heated with warm blankets and cosy cushions, fantastic gin cocktails and Alpine-inspired dishes of baked cheese with roasted vegetable and cured meats. Just the thing for banishing those winter blues!
Kick off your igloo experience with a seasonal cocktail made using Warner Edwards premium gin. Concoctions, designed to brighten up the greyest of winter days, include the Rhubarb Strudel, gin topped with toffee sauce, apple and nutmeg, Hugo with Warner Edwards elderflower gin, prosecco and apple juice and an uber elegant rhubarb martini.
Sharing boards, serving 2-3, include baked Camembert with roasted garlic, red onion and sourdough soldiers or a British charcuterie smorgasbord featuring air dried Oxsprings ham, Suffolk salami and chorizo.
And if this wasn't all enough, the Warner Edwards igloos are probably the best value in town with no hire charge when pre-ordering one of the fabulous group experiences on offer. Based on six sharing, packages start at just £45 for use of the igloo plus a cocktail for each guest, rising to £100 for a sharing board for up to six plus a cocktail each.
Book your Warner Edwards Igloo now by calling 020 8672 7018, or email castletooting@youngs.co.uk. Igloos will be open until the end of March.


text:
\section{Introduction}

The emission of active galactic nuclei (AGNs) is explained by the existence of a supermassive black hole (SMBH) at the centre of the host galaxy, which converts gravitational energy of material located in the surroundings into electromagnetic energy. This material forms a disk and loses angular momentum due to the viscosity in the disk, finally falling onto the black hole.
In general, the AGN spectra may show broad and narrow emission lines produced in regions close to the nucleus.
Sometimes they can also show lines from the host galaxy.
In radio-loud AGNs two plasma jets are ejected in direction perpendicular to the disc.

Among the different types of radio-loud AGNs, the objects called ``blazars" (BL Lacs and flat spectrum radio quasars, FSRQs) are powerful emitters from radio wavelengths up to $\gamma$-ray energies. They present strong flux variability and high and variable polarization \citep[e.g.][]{smi96}.
The most accepted scenario to explain these features suggests that we are observing the emission from a jet of material accelerated to relativistic velocities in the vicinity of the SMBH, and oriented very close to our line of sight. Thus the jet radiation is Doppler boosted and dominates over the other emission components from the nucleus (disc, broad line region - BLR, narrow line region) or host galaxy. The origin of the low-frequency radiation (radio to UV or X-ray band) from the jet is attributed to synchrotron emission and the high-energy radiation (X- to $\gamma$-rays) to an inverse-Compton process by the same relativistic electrons producing the synchrotron photons.
After the launch of satellites for high-energy observations such as the {\it Astrorivelatore Gamma ad Immagini Leggero} \citep[AGILE;][]{tav09} and {\it Fermi} \citep{abd09_fermi,atw09}, the number of sources detected at $\gamma$-rays has increased significantly, allowing a more detailed investigation of the high-energy processes occurring in blazars.

Among blazars, in general BL Lacs are objects of lower luminosity with featureless spectra or very weak emission lines. In contrast, FSRQs have higher luminosities and stronger emission lines.
\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{0827_IRop.eps}}
  \caption{Light curves of OJ~248 in optical ($R$ band) and near-IR ($J, H, K$ bands) in 2006--2013 built with GASP-WEBT data. In the near-IR light curves the blue diamonds are from the Campo Imperatore Observatory and the red points from the Teide Observatory.}
  \label{IR}
\end{figure}
In this paper, we present multifrequency observations of the FSRQ OJ~248 (0827+243) in 2006--2013 performed in the framework of a campaign led by the Whole Earth Blazar Telescope\footnote{http://www.oato.inaf.it/blazars/webt} (WEBT). The WEBT radio--optical observations are complemented by high-energy data from the {\it Swift} and {\it Fermi} satellites.

In the Roma BZCAT multi-frequency catalog of blazars\footnote{Edition 4.1.1, August 2012; http://www.asdc.asi.it/bzcat} \citep{mas09} OJ~248 appears with a redshift $z=0.939$ flagged as uncertain.
Mg II and Fe II absorption lines at $z=0.525$ were detected by \citet{ulr77} in the source optical spectrum. This intervening Damped Lyman $\alpha$ (DLA) system was subsequently studied by \citet{rao00}, who estimated a hydrogen column density $N_{\rm H} = (2.0 \pm 0.2) \times 10^{20} \rm \, cm^{-2}$. The DLA system is likely a disc galaxy with ongoing star formation \citep{ste02,rao03}. Although it does not affect the blazar photometry because of its faintness \citep{rao03}, its absorption of the source radiation must be taken into account.

OJ~248 was detected by the Energetic Gamma Ray Experiment Telescope (EGRET) instrument on board the {\it Compton Gamma Ray Observatory} (CGRO) with a variable flux.
In the third EGRET catalog of high-energy $\gamma$-ray sources \citep{har99} it appears with a flux $F(E>100 \rm \, MeV) = (24.9 \pm 3.9) \times 10^{-8} \, ph \, cm^{-2} \, s^{-1}$, single measurements ranging from 15.6 to $111.0 \times 10^{-8} \rm \, ph \, cm^{-2} \, s^{-1}$. It has $F(E>100 \rm \, MeV) = (5.3 \pm 0.5) \times 10^{-8} \, ph \, cm^{-2} \, s^{-1}$ and a spectral index $2.67 \pm 0.07$ in the Second Fermi-LAT catalog \citep[2FGL;][]{nol12}.
In the Nineties the source was very active also in the optical band \citep[e.g.][]{vil97,rai98a}.

\section[]{Optical and near-IR photometry}
\label{onir}

Optical photometric observations were provided in the $R$ band by several observatories participating in this WEBT project, including the GASP-WEBT collaboration and the Steward Observatory program in support of the {\it Fermi} $\gamma$-ray telescope \citep{smi09}.
They are:
 Abastumani (Georgia, FSU),
 Calar Alto\footnote{Calar Alto data was acquired as part of the MAPCAT project: http://www.iaa.es/$\sim$iagudo/research/MAPCAT} (Spain),
 Crimean (Ukraine),
 Lowell (Perkins telescope, USA),
 Lulin (Taiwan),
 Mt.\ Maidanak (Uzbekistan),
 Roque de los Muchachos (Liverpool telescope, Spain),
 Rozhen (Bulgaria),
 San Pedro Martir (Mexico),
 St.\ Petersburg (Russia),
 Steward (USA),
 Teide (IAC80 telescope, Spain),
 Tijarafe (Spain),
 Torino (Italy),
 Vidojevica (Serbia).

The period of interest goes from 2006 March
up to 2013 July.
We collected a total of 1356 data points, 1211 of which survived the light curve cleaning process, through which we discarded data with large errors as well as clear outliers.

In the light curve of Fig.~\ref{optical} we can see two major flaring periods, in 2006--2007 and 2012--2013. The first flare is of similar brightness ($R=15.6$) as that observed in November 1995 by \citet{rai98a}, which was a historical maximum.  The second outburst appears more prominent and shows a stronger variability. Two minor events are visible in 2009--2010 and in early 2011.

The 2007 peak was very sharp and was characterized by a brightening of $\sim 1.3$ mag in 11 days and about 1.0 mag fading in 9 days.
A noticeable variability also characterises the 2012--2013 outburst, with variations of about 1 mag in less than 6 days.
This can be compared with variations of 1.43 mag in 16 days observed by \citet{rai98a}, of 1.16 mag in 63 days observed by \citet{vil97}, and of 1.05 mag in 58 days reported by \citet{fan04}.
But the source also exhibits short-term variability.
In particular, we found a couple of changes of $\sim 0.3$ mag in about 7.5 hours in late 2012.
Intraday variability was previously reported by \citet{rai98a}, who observed a brightness decrease of 0.73 mag in 20 hours.

The GASP-WEBT near-IR data are collected in the $J, H, K$ bands at the Campo Imperatore (Italy) and Teide (TCS, Spain) observatories. Details on the data acquisition and reduction are given in \citet{rai14}.
A comparison between the $R$-band and near-IR source behaviour is shown in Fig.\ \ref{IR}.
Although the near-IR light curves are less sampled than the optical one, we can recognize the same main features, in particular the two outbursts of 2006--2007 and 2012--2013.
The variation amplitude increases with wavelength, as it is usually observed in FSRQs \citep[e.g.][]{rai12}, suggesting the presence of a ``stable" blue emission component, likely
thermal radiation from the accretion disc.

\section{Optical polarimetry}

Blazars are known to show variable polarization in both polarized flux percentage ($P$) and electric vector polarization angle (EVPA) \citep[e.g.][]{smi96}. In particular, wide rotations of the linear polarisation vector have been detected in a number of cases \citep{mar08,mar10,lar13,sorcia14}, which have been interpreted as the effect of motion along spiral trajectories.

Optical polarization data for this paper were provided by the Calar Alto, Crimean, Lowell, San Pedro Martir, St. Petersburg, and Steward observatories.
In Fig.\ \ref{pola} we show the time evolution of the polarization percentage $P$ compared with the $R$-band light curve.
For most of the time, the source showed low $P$ (average value of $\sim 3\%$), but during the brightening phase of the 2012--2013 outburst $P$ reached $\sim 19\%$, suggesting a correlation between $P$ and brightness typical of FSRQs \citep[e.g.][]{smi96,rai13}.
Figure \ref{polopt} shows $P$ versus the de-absorbed flux density in the $R$ band (see Sect.\ 8).
For any value of $F_R$ there is a large dispersion of $P$, but the highest values of $P$ ($>13\%$) are reached when the source is bright ($F_R > 1.3 \rm \, mJy$). The linear Pearson's correlation coefficient is 0.60, indicating a marginal correlation.

In order to investigate whether possible rotations of the linear polarisation vector occurred, we first examine the behaviour of the $Q$ and $U$ Stokes' parameters.
Figure \ref{stokes} shows that OJ~248 spent most of the time with $Q$ and $U$ being close to zero.  With this being the case, even small variations in $Q$ and $U$ necessarily lead to large EVPA rotations that are difficult to accurately follow unless the observations are very dense. The problem is mitigated during the 2012--2013 outburst, when $Q$ and $U$ exhibit large variations. This appears clearer in the $Q$ versus $U$ plot in Fig.\ \ref{q_u}, where subsequent data belonging to short time periods with good sampling have been connected to show the time evolution during the 2012--2013 outburst.
With this in mind, in Fig.\ \ref{pola_zoom} we finally plot the EVPA as a function of time during the outburst.
The $\pm \, n \pi$ ambiguity was fixed by assuming that the most likely value is that minimizing the angle variation, i.e.\
we added/subtracted 180\degr\ when needed to minimize the difference between subsequent points separated by less than 5 days.
It seems that there is not a preferable EVPA value and that the linear polarisation vector underwent wide rotations in both directions and with different ranges of angles. All this suggests a complex behaviour/structure of the magnetic field in the jet as is expected e.g.\ from a turbulent plasma flowing at a relativistic speed down the jet \citep{mar14}.

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=9cm]{pola.eps}}
  \caption{Time evolution of the optical magnitude in $R$ band (top panel) and of the percentage of polarized flux (bottom panel). The data are from different observatories: Calar Alto (green squares), Crimean (red diamonds), Lowell (pink asterisks), San Pedro Martir (cyan triangles), Steward (blue circles), and St. Petersburg (orange crosses).
}
  \label{pola}
\end{figure}

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{pol_opt_err.eps}}
  \caption{Optical polarization percentage $P$ plotted against the de-absorbed flux density in the $R$ band. The data are from different observatories: Calar Alto (green), Crimean (red), Lowell (pink), San Pedro Martir (cyan), Steward (blue), and St. Petersburg (orange).}
  \label{polopt}
\end{figure}

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{stokes.eps}}
  \caption{The evolution of the $Q$ and $U$ Stokes'parameters as a function of time. Different colours during the 2012--2013 outburst highlight the data of the selected periods indicated in Fig.\ \ref{q_u}.}
  \label{stokes}
\end{figure}

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{Q_U.eps}}
  \caption{$Q$ versus $U$ for all the data shown in Fig.\ \ref{stokes}. Coloured lines connect subsequent data belonging to the periods listed in the legend (JD-2450000). The direction is indicated by the arrows. }
  \label{q_u}
\end{figure}

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=9cm]{pola90_5.eps}}
  \caption{Time evolution of the optical magnitude in $R$ band (top panel), of the percentage of polarized flux (middle panel) and of the EVPA ``corrected" for the $\pm \, n
 \pi$ ambiguity (bottom panel, see text for explanation) during the 2012--2013 outburst. Data are from different observatories: Calar Alto (green squares), Crimean (red diamonds), Lowell (pink asterisks), San Pedro Martir (cyan triangles), Steward (blue circles), and St. Petersburg (orange crosses).
}
  \label{pola_zoom}
\end{figure}

\section{Optical spectroscopy}

Several previous studies found that there is no correlation between the jet activity and the behaviour of the broad emission lines in blazars \citep[see e.g.][]{cor00,rai07a}. Indeed, the BLR gas is likely ionized by the accretion disc radiation, whose variability is weaker and occurs on longer time scales than the variability of the beamed jet emission \citep[see e.g.][]{kas00}.
However, \citet{leo13} detected a flare-like variability of the Mg II emission line in the blazar 3C 454.3 during an outburst and claimed that the broad emission line fluctuations are linked to the non-thermal continuum emission from the jet.
With this in mind, we analyse the spectroscopic behaviour of OJ~248 during our monitoring period.

Optical spectra were taken at the Steward Observatory of the University of Arizona for the ``Ground-based Observational Support of the {\it Fermi} Gamma-ray Space Telescope" program\footnote{http://james.as.arizona.edu/$\sim$psmith/Fermi/}.
Data for this program are taken at the 2.3~m Bok telescope and 1.54~m Kuiper telescope \citep{smi09}; 140 spectra of OJ~248 were acquired during the first five cycles of the {\it Fermi} mission, from October 2008 to June 2013.

All spectra show a prominent Mg II $\lambda \lambda2796,2803$ broad emission line, which
was measured by fitting a Gaussian model with a single component, after
subtracting a linear fit to the continuum. We used  ad-hoc routines developed in IDL
and based on the MPFIT\footnote{http://www.physics.wisc.edu/$\sim$craigm/idl/fitting.html} libraries \citep{Markwardt09}.
The continuum region was selected from adjacent regions to the emission line, which are free of features.
The uncertainty of the measured flux was estimated from the average of the residuals obtained after the continuum fitting and was then used to determine the parameter confidence limits applying the routines in the MPFIT library.

In Fig.\ \ref{espectro} we show two of the spectra corresponding to different brightness states and in Fig.\ \ref{fit} the line and continuum fits as well as the residuals.
The results of the Mg II analysis are shown in Fig.\ \ref{graf_espectro}.
The line flux presents some dispersion around a mean value of $6.2 \times 10^{-15} \rm \, erg \, cm^{-2} \, s^{-1}$ with standard deviation of $0.5 \times 10^{-15} \rm \, erg \, cm^{-2} \, s^{-1}$. The possible presence of line variability can be checked e.g.\ by calculating the mean fractional variation
$f={{\sqrt{\sigma^2-\delta^2}} / {<F>}}$,
where $\sigma$ is the standard deviation, $\delta$ the mean square uncertainty of the fluxes, and $<F>$ the average flux \citep{pet01}.
The result is $f=0.08$, which means that the line flux is basically stable, and this is true also during the 2012--2013 outburst period, when the continuum flux increased by a factor $\sim 6$. Moreover, no delayed line flux increase was detected also after the outburst. Hence, the enhanced jet activity responsible for the outburst does not affect the BLR.

We measured the line full width at half-maximum\footnote{Corrected for the instrumental broadening of the line.} (FWHM), from which one can derive the velocity of the gas clouds in the BLR.
The average value is $v_{\rm FWHM} = 2053 \rm \, km \, s^{-1}$ with a standard deviation of $\sim 310 \rm \, km \, s^{-1}$.  The corresponding de-projected gas velocity, of course, depends on the geometry and orientation of the BLR \citep[see e.g.][]{dec11}.
In the blazar model, the BLR should be nearly face on, so measurements of FWHM are likely to be underestimated, since the measurement of the radial velocity will likely miss most of the orbital component.

In the bottom panel of Fig.\ \ref{graf_espectro} we finally plot the equivalent width (EW) versus the continuum flux density.
The EW decreases when the source brightens, which confirms that the jet is not the ionizing source of the BLR.
We notice that, according to the classical definition \citep{sti91}, blazars with rest-frame EW less than 5 \AA\ are classified as BL Lacs; in the case of OJ~248, this happens when the observed EW goes below 5 \AA $\times (1+z) \sim 9.7$ \AA, which occurs when the source continuum flux density around the Mg II line\footnote{We estimated the continuum flux density in the spectral regions 5320--5360 \AA\ and 5500--5530 \AA\ and then took the mean value.} exceeds $\sim 0.6 \times 10^{-15} \rm \, erg \, cm^{-2} \, s^{-1} \, \AA^{-1}$. This underlines the limit of the classical distinction between BL Lacs and FSRQs based on the EW, which depends on the source brightness.

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{0827_plot.eps}}
  \caption{Optical spectra of OJ~248 during different brightness states obtained at the Steward Observatory, showing the Mg~II emission line at $z=0.939$ (blue) and the Mg~II absorption line at $z=0.525$ (orange).}
  \label{espectro}
\end{figure}

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[angle=90]{fit.eps}}
  \caption{Gaussian fit (red solid line) to the Mg~II emission line of the spectrum taken on 2008 October 30 and shown in Fig.\ \ref{espectro}. The cyan line indicates the linear fit to the continuum; the red dashed line represents the residuals.}
  \label{fit}
\end{figure}

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{0827_Espectro.eps}}
  \caption{Top: time evolution of the Mg II broad emission line flux; the dashed line represents the average value and the dotted-dashed line the standard deviation around the mean. Bottom: EW of Mg II versus the continuum flux density; the solid line displays the behaviour of the EW assuming a constant line flux equal to its average value.}
  \label{graf_espectro}
\end{figure}

Fig.\ \ref{espectro} shows a strong absorption line at $\lambda=4270$ \AA\ due to Mg II absorption in the intervening DLA system at $z=0.525$ mentioned in the Introduction. We cannot perform a more detailed analysis of this line because the resolution of our spectra is about 20~\AA, implying a velocity resolution of $\sim 1400 \rm \, km \, s^{-1}$, while the FWHM of the Mg II absorption line is $\simeq 270 \rm \, km \, s^{-1}$ \citep{ste02}.

\section{Observations at radio and millimetre wavelengths}
\label{radiomm}

Radio and mm observations were performed with the Medicina (5, 8, and 22 GHz), Mets\"ahovi (37 GHz), Noto (43 GHz), IRAM (86 and 230 GHz), and Submillimeter Array (SMA, 230 and 345 GHz) telescopes.

A detailed description of the 43 GHz measurements performed with the Noto Radiotelescope can be found in \citet{let09}. For the Medicina observations, see e.g.\ \citet{bac07}.

The 37 GHz observations were made with the 13.7 m diameter Mets\"ahovi radio
telescope. The flux density scale is set by observations of DR 21. Sources NGC~7027,
3C~274 and 3C~84 are used as secondary calibrators. The error estimate in the flux
density includes the contribution from the measurement root mean square and the uncertainty
of the absolute calibration. A detailed description of the data reduction and analysis
is given in \citet{ter98}.

IRAM 30~m Telescope data were acquired as part of the POLAMI (Polarimetric AGN Monitoring with the IRAM 30~m Telescope) and MAPI (Monitoring AGN with Polarimetry at the IRAM 30~m Telescope) programs. Data reduction was performed following the procedures described in \citet{agu06,agu10}.

Millimetre and submillimetre data were also obtained at the Submillimeter Array (SMA) near the summit of Mauna Kea (Hawaii). OJ~248 is included in an ongoing monitoring program at the SMA to determine the fluxes of compact extragalactic radio sources that can be used as calibrators at mm wavelengths \citep{gur07}. OJ~248 was also observed as part of a dedicated program to follow sources on the {\it Fermi} LAT Monitored Source List (PI: A. Wehrle) in 2009 and 2010. In the ongoing monitoring sessions, available potential calibrators are observed for 3 to 5 minutes, and the measured source signal strength calibrated against known standards, typically solar system objects (Titan, Uranus, Neptune, or Callisto). In addition, from time to time calibrator data obtained during regular science observations are also used to obtain flux density measurements. Data from this program are updated regularly and are available at the SMA website\footnote{http://sma1.sma.hawaii.edu/callist/callist.html}.

\begin{figure*}
\centering
\includegraphics[width=14cm]{0827_radioopt.eps}
  \caption{Light curves of OJ~248 at different frequencies in 2006--2013. From top to bottom: $R$-band optical magnitudes (see also Fig.\ \ref{optical}), 345 GHz data from SMA, 230 GHz data from SMA (red triangles) and IRAM (blue crosses), 86 GHz data from IRAM, 43 GHz data from Noto, 37 GHz data from Mets\"ahovi, 22, 8, and 5 GHz data from Medicina.}
  \label{radio}
\end{figure*}

As one can see in Fig.\ \ref{radio}, the mm data (230 and 86 GHz) show two prominent outbursts of the same strength peaking in late 2010 and early 2013.
Going to lower frequency (37 GHz), the second outburst becomes fainter than the first, and it completely disappears at 8 GHz. A comparison with the optical light curve suggests that the 2013 mm--radio outburst is the time delayed counterpart of the 2012--2013 optical event, while a possible correlation between the optical and radio variations in correspondence of the 2010--2011 mm--radio outburst is more difficult to establish. Indeed, there are no visible optical flares either contemporaneous or slightly preceding the lower-frequency outburst, but just one event
about one year before, which however is more likely connected with the pre-outburst bumps visible at 230 and 37 GHz. In fact, there is a definite rise in the 230 GHz light curve that starts at essentially the same time as the late 2009--early 2010 optical event.
Most likely the more or less prominent optical counterpart of the main mm--radio outburst remained unobserved due to the 2010 seasonal gap: indeed, some residual activity can be seen at the start of the subsequent observing season.
The 2006--2007 optical outburst might be correlated with a minor radio event observed a few months later at 86 (and 230) GHz.
We used the discrete correlation function \citep[DCF;][]{ede88,huf92} to analyse cross-correlations among light curves. Figure \ref{dcf_radio} shows the DCF between the optical de-absorbed (see Sect.\ \ref{asso}) and 230 GHz flux densities. The peak value is 0.8, which implies good correlation, and the time delay corresponding to the peak is 28 days, which would be the time lag of the mm variations after the optical ones. However, this result is dominated by the last outburst and the DCF run on the pre-outburst period gives no significant signal.

Flares can be produced by shocks propagating downstream the jet and/or by variations of the Doppler factor $\delta$, which depends on both the bulk Lorentz factor of the relativistic plasma, $\Gamma_{\rm b}$, and the viewing angle $\theta$,
$\delta=[\Gamma_{\rm b} \, (1-\beta \, \cos\theta)]^{-1}$, where $\beta$ is the velocity in units of the light speed.
The different behaviour of OJ~248 in various epochs, i.e.\ different correlation between optical and radio variations, can be explained in terms of a misalignment of the region emitting the bulk of the optical radiation with respect to the zone emitting the bulk of radio photons \citep[see e.g.][]{vil07,vil09b,vil09a,rai11}.
The radiation coming from the jet region with a smaller viewing angle will in fact be more Doppler boosted. According to this interpretation, in 2010--2011 the radio emitting region was more aligned with the line of sight than the optical zone, while in 2012--2013 the most external jet regions, emitting the low-frequency radio photons, had a larger viewing angle, and the strong optical outburst was the effect of a viewing angle smaller than ever.

We finally notice that there is a time delay of the radio flux variations going toward longer wavelengths; in particular, by means of the DCF we could estimate the time lag between the 230 and 37 GHz flux changes  (see Fig.\ \ref{dcf_radio}). The peak of the DCF is strongly asymmetric, so that a better estimate of the delay in this case is given by the centroid of the distribution \citep{pet98}, which indicates a value of 40--50 days. Moreover, the amplitude of the flux variations decreases at lower frequencies (the ratio between the maximum and minimum flux density is $\sim 24$ at 230 GHz, 7.4 at 86 GHz, and 6.3 at 37 GHz), and the light curves become smoother with longer-lasting events.
This is what we expect if the radio emission at longer wavelengths comes from more external (because of synchrotron self-absorption) and more extended regions of the jet.

An alternative picture to explain the radio--optical variability is in terms of a disturbance, e.g.\ shock wave, propagating downstream the jet where the delay from high radio frequencies towards low radio frequencies is naturally caused by opacity effects.
In case the optical and mm emitting regions are co-spatial, the reason why the mm peak is time delayed may be due to a rather high lower-energy cutoff to the electron energy distribution in the early stages of the outburst.
\begin{figure}
\includegraphics[width=8.5cm]{dcf_radio.eps}
  \caption{Discrete correlation functions between the $R$-band de-absorbed and 230 GHz flux densities (blue filled circles) and between the 230 and 37 light curves (red empty circles).}
\label{dcf_radio}
\end{figure}

\section{{\it Swift} observations}

The {\it Swift} satellite \citep{geh04} carries three instruments that work simultaneously in different frequency ranges: the X-Ray Telescope (XRT), observing between 0.3 and 10 keV \citep{bur05}, the Ultraviolet-Optical Telescope (UVOT), between 170 and 600 nm \citep{rom05}, and the Burst Alert Telescope (BAT), between 14 and 195 keV \citep{bar05}.
OJ~248 was observed by {\it Swift} 86 times between 2008 January and 2013 May.

\subsection{UVOT observations}
\label{uvo}

The UVOT telescope can acquire data in optical ($v, b, u$) and UV ($w1, m2, w2$) bands \citep{poo08}.
The data reduction was performed with the {\sevensize \bf HEASoft} package version 6.13 and the Calibration Database (CALDB) 20130118 of the NASA's High Energy Astrophysics Science Archive Research Center\footnote{http://heasarc.gsfc.nasa.gov} (HEASARC). We extracted the source counts within a 5 arcsec radius aperture and the background counts from a nearby circular region with 15 arcsec radius. We summed multiple observations in the same filter with the {\tt uvotimsum} task and then processed them with {\tt uvotsource}.

The resulting light curves are shown in Fig.~\ref{uvot}. No observations were available in the $b$ band. After 2010.0 the difference between the maximum and minimum magnitudes in the different bands is 1.12 in $w2$, 1.05 in $m2$, 1.15 in $w1$, 1.25 in $u$. It is 0.67 in $v$, but in this case we have only four points. We can see that the variability in general decreases when the frequency increases, extending the trend we noticed in Sect.\ \ref{onir} for the optical and near-IR light curves.

\begin{figure}
  \scalebox{1.0}{\includegraphics[width=8.5cm]{0827_UV.eps}}
  \caption{Light curves of OJ~248 built with {\it Swift}-UVOT data in optical and UV.}
  \label{uvot}
\end{figure}

\subsection{XRT observations}

Reduction of the XRT data was performed with the {\sevensize \bf HEASoft package} version 6.13 with the calibration file 20130313. There are 83 observations in photon-counting (PC) mode. We ran the task {\tt xrtpipeline} with standard screening criteria.
For further analysis we only kept the 64 observations with more than 50 counts.
Source counts were extracted with the {\tt xselect} task from a circular region of 30 pixel radius centred on the source and the background counts were derived from a surrounding annular region of 50 and 70 pixel radii. No correction for pile-up was needed since the count rate is always lower than 0.5 counts/s. We performed spectral fits with the {\sevensize \bf Xspec} package in the 0.3--10 keV energy range, using the Cash statistics because of the low count number.
We modelled the spectra with a power law with photoelectric absorption, adopting a hydrogen atomic column density $N_{\rm H}=4.6 \times 10^{20} \rm \, cm^{-2}$ obtained by summing the Galactic value $2.6 \times 10^{20} \rm \, cm^{-2}$ \citep{kal05} to that of the intervening DLA system at $z=0.525$ \citep{rao00}.

The X-ray spectrum acquired on 2012 October 2 is shown in Fig.~\ref{xrt} as an example. It was best-fitted with a power law with photon index $\Gamma=1.49 \pm 0.10$.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[angle=-90]{02_oct_2012.eps}}
  \caption{The XRT spectrum of OJ~248 on 2012 October 2. The best fit was obtained with a power law with fixed absorption given by the sum of the Galactic and intervening DLA $N_{\rm H}$ values. The bottom panel shows the ratio of the data to the folded model.}
\label{xrt}
\end{figure}

In Fig.~\ref{xrtgamma} we plotted $\Gamma$ as a function of the flux density at 1 keV for the 58 observations with error less than 30\% of the flux. The values of $\Gamma$ range between 1.06 and 2.07, with an average value of 1.65 and no significant trend of $\Gamma$ with flux, in contrast to the harder-when-brighter trend sometimes found in FSRQs \citep[e.g.][]{ver10}.
The smaller dispersion of the data points corresponding to the 2012--2013 outburst (standard deviation $\sigma=0.09$) with respect to the pre-outburst data ($\sigma=0.24$) is likely due to their higher precision because of the larger count number. In both cases the standard deviation is less than the average error (0.16 and 0.29, respectively), indicating that the data are consistent with a constant value.

\begin{figure}
\includegraphics[width=8.5cm]{gamma.eps}
  \caption{The X-ray photon index $\Gamma$ as  a function of the unabsorbed flux density at 1 keV. Only data with error less than 30\% of the flux are shown. Red points correspond to data acquired after $\rm JD=2456100$, i.e.\ during the 2012--2013 outburst.}
\label{xrtgamma}
\end{figure}

Notice that
\citet{jor04} analysed Chandra data using $N_{\rm H}= 3.62 \times 10^{20} \rm \, cm^{-2}$, i.e.\ the Galactic value according to \citet{dic90}, and that
\citet{str13} found a value of $N_{\rm H}= (7\pm 2) \times 10^{20} \rm \, cm^{-2}$ when analysing XRT data with an absorbed power law with freely varying $N_{\rm H}$.

The resulting X-ray light curve (flux densities at 1 keV) is shown in Fig.\ \ref{multi}, where it is compared to the source behaviour at other frequencies.

\section{{\it Fermi} observations}

\begin{table*}
 \centering
  \caption{Results of the spectral analysis of the {\it Fermi}-LAT data of OJ~248 in the 0.1--100 GeV energy range. The reference energy $E_{\rm 0}$ was fixed to 392.1 MeV. The fitted model was a power law with photon index $\Gamma$.}
   \label{fermitab}
  \begin{tabular}{@{}crrcr@{}}
  \hline
Date &  $N_{\rm pred}$  &TS & $\Gamma$ & $F_{\rm 0.1-100 GeV}$ \\
     &                  &   &          & $[10^{-8} \rm \, ph \, cm^{-2} \, s^{-1}]$ \\
 \hline
2008 Aug 04 - 2009 Mar 05 &539 & 125 & $2.77 \pm 0.12$ & $6.2 \pm 0.8$\\
2009 Mar 05 - 2009 Oct 15 &465 & 131 & $2.55 \pm 0.11$& $5.2 \pm 0.8$\\
2009 Oct 15 - 2010 May 27 &406 & 104 & $2.60 \pm 0.12$& $5.3 \pm 0.8$\\
2010 May 27 - 2011 Jan 05 &466 & 100 & $2.83 \pm 0.12$& $6.6 \pm 0.9$\\
2011 Jan 06 - 2011 Aug 18 &439 & 97 & $2.81 \pm 0.13$& $6.4 \pm 1.0$\\
2011 Aug 18 - 2012 Feb 02 &283 & 43 & $3.13 \pm 0.23$& $5.5 \pm 1.0$\\
2012 Feb 02 - 2012 Jul 19 &392 & 107 & $2.66 \pm 0.13$& $6.9 \pm 1.0$\\
2012 Jul 19 - 2013 Jan 03 &1975 & 2106 & $2.38 \pm 0.03$& $31.5 \pm 1.3$\\
2013 Jan 03 - 2013 Jun 20 &730 & 401 & $2.48 \pm 0.07$& $12.6 \pm 1.1$\\
2013 Jun 20 - 2013 Nov 08 &313 & 103 & $2.56 \pm 0.13$& $6.5 \pm 1.1$\\
\hline
\end{tabular}
\end{table*}

The {\it  Fermi} satellite  was launched on 2008 June 11. Its aim is to perform a daily mapping of the $\gamma$-ray sources in the Universe.
The primary instrument of {\it Fermi} is the Large Area Telescope \citep[LAT;][]{atw09}.
The energy range covered is approximately from 20 MeV to more than 300 GeV. The field of view of the LAT covers about 20\% of the sky, and maps all the sky every three hours.

The data in this paper were collected from 2008 August 4 ($\rm JD=2454683$) to 2013 November 8 ($\rm JD=2456605$). We performed the analysis with the {\sevensize \bf SCIENCETOOLS} software package version v9r32p5. The data were extracted within a Region of Interest (ROI) of 10\degr\ radius and a maximum zenith angle of 100\degr\ to reduce contamination from the Earth limb $\gamma$-rays, which are produced by cosmic rays interacting with the upper atmosphere. Only events belonging to the `Source' class were used. The time intervals when the rocking angle of the LAT was greater than 52\degr\ were rejected. For the spectral analysis we used the science tool {\tt gtlike} with the response function {\tt P7REP\_SOURCE\_V15}.
Isotropic (iso\_source\_v05.txt) and Galactic diffuse emission
(gll\_iem\_v05.fit) components were used to model the
background\footnote{http://fermi.gsfc.nasa.gov/ssc/data/access/lat/\\BackgroundModels.html}.

We evaluated the significance of the $\gamma$-ray signal from the sources within the ROI by means of the Test Statistics  $\rm TS = 2 \, (\log L_1 - \log L_0)$, where $L_1$ and $L_0$ are the likelihood of the data given the model with or without the source, respectively \citep{mat96}. As was done in the 2FGL catalog \citep{nol12}, for the spectral modelling of OJ~248 we adopted a power law, $N(E)= N_{\rm 0} \, (E/E_{\rm 0})^{-\Gamma}$, where $E_{0}=392.1$ MeV is the reference energy between 0.1 and 100 GeV. We first ran {\tt gtlike} with the {\tt DRMNFB} optimizer, including all point sources of the catalog within 15\degr\ from our target, and using power-law fits to model the spectra of these sources. We then ran {\tt gtlike} a second time with {\tt NEWMINUIT} as optimizer, after selecting the sources with $\rm TS > 10$ and the predicted number of counts $N_{\rm pred}>3$.

The results of the analysis are reported in Table \ref{fermitab} for time bins of about six months.
The average photon index is 2.68, and its standard deviation is 0.22.
This value is essentially the same as that reported in the 2FGL catalog ($2.67 \pm 0.07$),
while an analysis over the whole period considered in this paper yields $\Gamma= 2.56 \pm 0.03$
and a flux of $(8.6 \pm 0.3) \times 10^{-8} \, \rm  ph \, cm^{-2} \, s^{-1}$.
The photon index variability is dominated by errors, since the variance $\sigma^2$ is smaller than the mean square uncertainty $\delta^2$ (see Sect.\ 4).
In Fig.\ \ref{multi} we can see the corresponding $\gamma$-ray light curve (red points).
We also plotted a monthly-binned light curve (blue points) that includes many upper limits (cyan points) because of the source faintness. Finally, during the 2013 outburst we performed weekly bins when there was a good count number to detail the flux variations (green points).

\begin{figure*}
\centering
\includegraphics[width=14cm]{0827_mult.eps}
  \caption{Light curves of OJ~248 at different frequencies in 2006--2013.
From top to bottom: the {\it Fermi}-LAT 0.1--100 GeV fluxes ($10^{-8} \rm \, ph \, cm^{-2} \, s^{-1}$) derived with different time bins (red symbols refer to data binned over roughly six-month time intervals, blue ones to monthly binned data, and green symbols to weekly-binned data in the outburst period; cyan arrows indicate upper limits); the 1-keV {\it Swift}-XRT flux densities ($\mu$Jy); the {\it Swift}-UVOT $m2$ flux densities (mJy); the GASP-WEBT $R$-band flux densities (mJy); the GASP-WEBT $K$-band flux densities (mJy); the 230 GHz flux densities (Jy); the 37 GHz (orange points) and 43 GHz (green points) flux densities (Jy). The X-ray, UV, optical and near-IR light curves were corrected by both Galactic and DLA absorption.}
\label{multi}
\end{figure*}

\section{Correction for Galactic and DLA extinction}
\label{asso}

In the previous sections we presented light curves of OJ~248 as observed magnitudes.
But the near-IR, optical, and UV radiation from the source suffers absorption by both the Galaxy dust and the dust contained in the intervening DLA system at $z=0.525$ mentioned in the Introduction. This is a problem similar to that met when analyzing data from another well-known blazar, AO 0235+16 \citep{rai05}.

We estimated the Galactic reddening in the $UBVRIJHK$ optical and near-IR bands by using the \citet{car89} extinction law, with $R_V=A_V/E(B-V)=3.1$, which is the standard value for the diffuse interstellar medium.
The results are reported in Table \ref{ext} (Column 2).
An estimate of the extinction due to the DLA system can be calculated starting from the hydrogen column density $N_H=(2.0 \pm 0.2) \times 10^{20} \rm \, cm^{-2}$ obtained by \citet{rao00} and adopting a gas-to-dust ratio equal to the average value in the Milky Way: $N_H=4.93 \times 10^{21} {\rm \, cm^{-2} \, mag^{-1}} \times E(B-V)$ \citep{dip94}. This yields $E(B-V)=0.04$, and assuming again $R_V=3.1$, we obtain $A_V=0.124$ at $z=0.525$.
Then, by applying the same \citet{car89} law properly blueshifted, we get
the values reported in Table \ref{ext} (Column 3).
We note that the DLA system is a more important absorber than the Galaxy.
The assumption that the DLA system has the same absorbing characteristics of the Milky Way is justified by its being a spiral galaxy \citep{rao03}.
The values of the total extinction that we must apply to correct our data for absorption in both the Galaxy and the DLA system are given in Column 4.

In the case of the {\it Swift}-UVOT bands, because of the asymmetric shape of the filter responses and of the bumped shape of the extinction law in the UV, we calculated the absorption in the various bands by integrating the \citet{car89} law with the filter effective areas \citep[see e.g.][]{rai10}. The results are shown in Table \ref{ext}.

\begin{table}
 \centering
  \caption{Extinction [mag] in the various Bessel \citep{bes98} and {\it Swift}-UVOT bands toward OJ~248.
Both the Galactic absorption and that by the DLA system at $z=0.525$ are given.
The value of the total extinction suffered by the source radiation is the sum of the two.}
   \label{ext}
  \begin{tabular}{@{}cccc@{}}
  \hline
Band & $A_\lambda$(Gal) & $A_\lambda$(DLA) & Total\\
 \hline
\multicolumn{4}{c}{{\it Swift}-UVOT bands}\\
$w2$ & 0.249 & 0.397 & 0.646\\
$m2$ & 0.261 & 0.343 & 0.604\\
$w1$ & 0.211 & 0.331 & 0.542\\
$u$ & 0.150 & 0.349 & 0.499\\
$b$ & 0.125 & 0.240 & 0.365\\
$v$ & 0.095 & 0.196 & 0.291\\
\hline
\multicolumn{4}{c}{Bessel bands}\\
$U$ & 0.142 & 0.316 & 0.458\\
$B$ & 0.122 & 0.235 & 0.357\\
$V$ & 0.093 & 0.195 & 0.288\\
$R$ & 0.077 & 0.173 & 0.250\\
$I$ & 0.055 & 0.131 & 0.186\\
$J$ & 0.027 & 0.074 & 0.101\\
$H$ & 0.017 & 0.045 & 0.062\\
$K$ & 0.011 & 0.028 & 0.039\\
\hline
\end{tabular}
\end{table}

\section{Cross-correlation between variability at high and low energies}

In order to better investigate the relationship between the source behaviour in $\gamma$-rays and that in the optical band, we show in Fig.\ \ref{zoom} the corresponding whole light curves as well as an enlargement of the 2012--2013 outburst period, where the correlation is easier to study. The start of the $\gamma$-ray outburst is not covered in the optical band because of the solar conjunction, but the first point after the seasonal gap is about 0.3 mag brighter than before, suggesting that the outburst has already begun.
In contrast, the optical light curve is very well sampled in the outburst decline phase, where the $\gamma$-ray curve has a worst time resolution because of the low flux.
It seems that the $\gamma$ and optical fluxes may well have risen and declined together, but that the period of major $\gamma$ activity preceded the phase of strongest optical activity.

To get a quantitative estimate of this time shift, we calculate the DCF (see Sect.\ \ref{radiomm}) between the $\gamma$-ray fluxes and the $R$-band flux densities corrected for the total absorption reported in Table \ref{ext}\footnote{We considered the weekly $\gamma$ fluxes during the outburst period, and the monthly fluxes before and after that (see Fig.\ \ref{zoom}), while we binned the optical data in seven-day bins.}.
The DCF is displayed in Fig.\ \ref{cross}. It shows a peak at a lag of $\tau_{\rm p} = 28$ days with $\rm DCF_{p} = 1.3$ that indicates strong correlation with the optical variations following the $\gamma$-ray ones after four weeks. The delay is 29 days if we take the centroid instead of the peak.
The figure inset displays the result of 2000 Monte Carlo simulations according to the ``flux randomization-random subset selection" method \citep{pet98,rai03}.
From these simulations it is possible to estimate the uncertainty on the delay.
We obtained that 88\% of the realizations led to a centroid value between 22 and 36 days.
Hence, we infer that  the optical flux variations follow the $\gamma$ flux changes with a delay of  $29 \pm 7 \rm \, days$.

However, if the $\gamma$ emission is due to inverse-Compton scattering of soft photons off the same electrons producing the optical radiation, then its variations are expected to be simultaneous or delayed with respect to those characterising the optical radiation, as resulting from
modelling non-thermal flares with shocks in a jet \citep[e.g.][]{sikora01,sokolov04,sokolov05}. This was observed in several blazars, in particular in the FSRQs 4C~38.41 \citep{rai12}, 3C~345 \citep{schinzel12}, and 3C~454.3 \citep{bon09,ver10,rai11}.
In contrast, $\gamma$ variations leading the optical ones were observed e.g.\ in the FSRQs PKS~1510-09 by \citet{abdo10_1510} and \citet{dam11}, and 3C~279 by \citet{hay12}. The latter authors found a lag of about 10 days and explained it by assuming that the energy density of the external seed photons for the inverse-Compton process decreases faster along the jet than the energy density of the magnetic field causing the synchrotron optical emission \citep[see also][]{janiak12}. Analogous interpretations may also hold for OJ~248.

Alternatively, the complex optical/$\gamma$-ray correlation may be explained by considering the effects of turbulence in the jet \citep{mar14}.
The fluctuating magnitude and direction of a turbulent magnetic field affects mostly the synchrotron radiation, and therefore adds a component to the optical variability that is not present in the gamma-ray light curve.

Figure \ref{cross} also displays the DCF between the $\gamma$-ray fluxes and the X-ray flux densities at 1 keV, suggesting a delay of the X-ray variations of about 2 months. We finally investigated the $\gamma$-mm correlation, finding a strong signal and a $\sim 70$ days delay of the mm variations.

\begin{figure}
\includegraphics[width=8.5cm]{0827_gamop.eps}
  \caption{Light curves in the $\gamma$-ray and optical ($R$) bands over the whole period (top), and during the 2012--2013 outburst period indicated by the yellow stripe (bottom).}
\label{zoom}
\end{figure}

\begin{figure}
\includegraphics[width=8.5cm]{dcf_gow.eps}
  \caption{Discrete correlation functions between the $\gamma$-ray fluxes and the $R$-band de-absorbed flux densities (blue filled circles) and between the $\gamma$-ray fluxes and the X-ray flux densities at 1 keV (red empty circles). The inset shows the results of Monte Carlo simulations of the $\gamma$-optical correlation (see text for details).}
\label{cross}
\end{figure}

Another interesting correlation holds between the X-ray and mm flux densities. Indeed, beside the 2012--2013 outburst, the X-ray light curve also shows a peak during the maximum of the mm light curve at the end of 2010 (see Fig.\ \ref{multi}). The DCF in Fig.\ \ref{xmm} displays a strong correlation with no time lag, which suggests that the X-ray and mm radiation are produced in the same region, with the X-ray emission likely due to inverse-Compton on the mm photons.
A correlation between the X-ray and mm variability has already been found, e.g.\ in BL Lacertae \citep{rai13}.

In Fig.\ \ref{xmm} we also show the DCF between the X-ray and optical flux densities, indicating that the optical variations precede those in the X-rays by about one month.

Cross-correlations of the $\gamma$-ray, X-ray, and $R$-band data with the 37 GHz data only led to weak and somewhat confused signals. This is due to the different behaviour of the corresponding light curves, in particular to the dominance of the 2010--2011 outburst with respect to the 2013 one at 37 GHz.

\begin{figure}
\includegraphics[width=8.5cm]{dcf_xmm.eps}
  \caption{Discrete correlation functions between the X-ray and 230 GHz flux densities (blue filled circles) and between the X-ray and $R$-band de-absorbed flux densities (red empty circles).}
\label{xmm}
\end{figure}

\section{Broad-band SED}

Three broad-band SEDs of OJ~248 are plotted in Fig.\ \ref{sed}.
They correspond to the peak of the $\gamma$-ray emission ($\rm JD=2456284$), to the peak of the X-ray emission ($\rm JD=2456317$), and to a faint post-outburst epoch ($\rm JD=2456368$).
The SEDs are built with simultaneous near-IR, optical, UV, X-ray, and $\gamma$-ray data.
Because of the smoother radio variability, we gave a tolerance of a few days to the radio data.

Emission in the optical--UV receives an important contribution from the accretion disc radiation, whose signature is more evident in the faint, post-outburst SED. The concave shape of the near-IR spectrum is due to the intersection between the disc contribution and the non-thermal jet emission. These two components have been modelled by \citet{rai14}, who found that the OJ~248 disc is more luminous than a typical type 1 QSO disc.

Notice that the faintest SED at high energies has also the lowest radio flux at 230 GHz, but it exceeds the fluxes of the other SEDs at longer radio wavelengths.

\begin{figure*}
\centering
\includegraphics[width=14cm]{sed_0827.eps}
  \caption{Spectral energy distributions of OJ~248 from the radio to the $\gamma$-ray frequencies during three epochs characterised by different brightness states.}
\label{sed}
\end{figure*}

\section{Summary and Conclusions}

In this paper we have presented the results of a huge multiwavelength observing effort led by the GASP-WEBT Collaboration on the blazar OJ~248. Data were collected starting from 2006 and up to 2013, including two optical-NIR outbursts in 2006--2007 and 2012--2013 and two major radio outbursts in 2010--2011 and 2012--2013. The 2012--2013 outburst was also detected at high energies by the {\it Swift} and {\it Fermi} satellites. The correlation between the optical and radio outbursts is clear in 2012--2013, while the optical counterpart of the 2010--2011 radio outburst is difficult to identify. Something likely changed in the source in the period between the two outbursts, one possibility being a slightly better alignment of the optical emitting region with the line of sight with the consequent increase of the Doppler beaming.
A strong correlation between the flux variations at $\gamma$-rays and those in the optical band is found, but with the optical variations delayed by about one month, which is a peculiar behaviour already found in other blazars. Strong correlation with no time delay has also been found between the X-ray and millimetre flux changes, supporting a common emission region in the jet.

We have analysed the polarimetric behaviour of the source. The fraction of polarised flux remained low for most of time but during the 2012--2013 outburst, when $P$ reached $\sim 19\%$. Wide rotations of the linear polarisation vector can reliably be detected only during the outburst and they occur in both directions, suggesting a complex behaviour of the magnetic field in the jet possibly due to turbulence, and/or a complex jet structure involving spiral paths.

Optical spectra show Mg~II lines both in absorption and emission. The absorption line is due to an intervening system at z=0.525 whose reddening effects on the NIR, optical, and UV source emission have been estimated and taken into account. The presence of the intervening system must be considered also when analysing the X-ray radiation. As for the Mg~II emission line from the source BLR, we estimated a mean velocity of $(2053 \pm 310) \rm \, km \, s^{-1}$. The line flux is essentially stable around a mean value of $(6.2 \pm 0.5) \times 10^{-15} \rm \, erg \, cm ^{-2} \, s^{-1}$ also during the 2012--2013 outburst and after, confirming that the jet emission did not affect the BLR, even when considering up to a few months of possible time delay.

\section*{Acknowledgments}
The data collected by the GASP-WEBT collaboration are stored in the GASP-WEBT archive; for questions regarding their availability, please contact the WEBT President Massimo Villata ({\tt villata@oato.inaf.it}).
We thank the referee, Vasiliki Pavlidou, for useful comments and suggestions.
This article is partly based on observations made with the telescopes IAC80 and TCS operated by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide on the island of Tenerife. Most of the observations were taken under the rutinary observation program. The IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide.
St.Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St.Petersburg University research grant 6.38.335.2015.
AZT-24 observations are made within an agreement between  Pulkovo, Rome and Teramo observatories.
The Abastumani team acknowledges financial support of the project
FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under
contract 31/77.
This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC.
Acquisition and reduction of the MAPCAT and IRAM 30 m data is supported in part by MINECO (Spain) grant and AYA2010-14844, and by CEIC (Andaluc\'{i}a) grant P09-FQM-4784.
This paper is partly based on observations carried
out at the IRAM 30 m Telescope, which is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica.
The Steward Observatory spectropolarimetric monitoring project is supported by the Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G.
The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX11AQ03G and NNX13AO99G.
The PRISM camera at Lowell Observatory was developed by K.\ Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory.
The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the
Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with funding
from the UK Science and Technology Facilities Council.
The Mets\"ahovi team acknowledges the support from the Academy of Finland
to our observing projects (numbers 212656, 210338, 121148, and others).
Partly based on observations with the Medicina and Noto telescopes
operated by INAF - Istituto di Radioastronomia.
E.~ B.\ acknowledge financial support from UNAM-DGAPA-PAPIIT
through grant IN111514.
GD and OV did the observations/investigations in line with Projects No. 176011 (Dynamics and Kinematics of Celestial Bodies and Systems), 176021 (Visible and Invisible Matter in Nearby Galaxies: Theory and Observations) and 176004 (Stellar Physics) which are supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia.
The Torino team acknowledges financial support by INAF through contract PRIN-INAF 2011.

redpajama_set_name: RedPajamaArXiv


Indeed, some wifi routers are already appearing on the market with locked firmware, since that is simply much cheaper for manufacturers to do, than attempt to follow the FCC's proposed regulation. (I.e. a chilling effect.) You can read more about this pending regulation at Prpl.works, Ars Technica, Wired, and Libreplanet. The motivation behind the FCC's proposed rules to is better address abuse of the Wifi spectrum, however the proposed rules would effect far more people than those who have been found to be misusing Wifi.
At any rate, we think these proposed rules are a really bad idea! Besides WasabiNet, such regulation would also stifle innovation, tinkering, academic research, other community networking groups like Freifunk, and even grant-funded groups like the New America Foundation's OTI.
If you disagree with this pending regulation, you can file a comment to the FCC youself before October 9, 2015! This page from Libreplanet offers more info and tips about filing comments.
Additionally, you can search previously filed comments to the FCC for reference (beware, link seems to go down periodically).