text:
var ac_polyfills =
/******/ (function(modules) { // webpackBootstrap
/******/ 	// install a JSONP callback for chunk loading
/******/ 	var parentJsonpFunction = window["webpackJsonpac__name_"];
/******/ 	window["webpackJsonpac__name_"] = function webpackJsonpCallback(chunkIds, moreModules, executeModules) {
/******/ 		// add "moreModules" to the modules object,
/******/ 		// then flag all "chunkIds" as loaded and fire callback
/******/ 		var moduleId, chunkId, i = 0, resolves = [], result;
/******/ 		for(;i < chunkIds.length; i++) {
/******/ 			chunkId = chunkIds[i];
/******/ 			if(installedChunks[chunkId])
/******/ 				resolves.push(installedChunks[chunkId][0]);
/******/ 			installedChunks[chunkId] = 0;
/******/ 		}
/******/ 		for(moduleId in moreModules) {
/******/ 			if(Object.prototype.hasOwnProperty.call(moreModules, moduleId)) {
/******/ 				modules[moduleId] = moreModules[moduleId];
/******/ 			}
/******/ 		}
/******/ 		if(parentJsonpFunction) parentJsonpFunction(chunkIds, moreModules, executeModules);
/******/ 		while(resolves.length)
/******/ 			resolves.shift()();
/******/ 		if(executeModules) {
/******/ 			for(i=0; i < executeModules.length; i++) {
/******/ 				result = __webpack_require__(__webpack_require__.s = executeModules[i]);
/******/ 			}
/******/ 		}
/******/ 		return result;
/******/ 	};

/******/ 	// The module cache
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/******/ 	// objects to store loaded and loading chunks
/******/ 	var installedChunks = {
/******/ 		2: 0
/******/ 	};

/******/ 	// The require function
/******/ 	function __webpack_require__(moduleId) {

/******/ 		// Check if module is in cache
/******/ 		if(installedModules[moduleId])
/******/ 			return installedModules[moduleId].exports;

/******/ 		// Create a new module (and put it into the cache)
/******/ 		var module = installedModules[moduleId] = {
/******/ 			i: moduleId,
/******/ 			l: false,
/******/ 			exports: {}
/******/ 		};

/******/ 		// Execute the module function
/******/ 		modules[moduleId].call(module.exports, module, module.exports, __webpack_require__);

/******/ 		// Flag the module as loaded
/******/ 		module.l = true;

/******/ 		// Return the exports of the module
/******/ 		return module.exports;
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/******/ 	// This file contains only the entry chunk.
/******/ 	// The chunk loading function for additional chunks
/******/ 	__webpack_require__.e = function requireEnsure(chunkId) {
/******/ 		if(installedChunks[chunkId] === 0)
/******/ 			return Promise.resolve();

/******/ 		// an Promise means "currently loading".
/******/ 		if(installedChunks[chunkId]) {
/******/ 			return installedChunks[chunkId][2];
/******/ 		}
/******/ 		// start chunk loading
/******/ 		var head = document.getElementsByTagName('head')[0];
/******/ 		var script = document.createElement('script');
/******/ 		script.type = 'text/javascript';
/******/ 		script.charset = 'utf-8';
/******/ 		script.async = true;
/******/ 		script.timeout = 120000;

/******/ 		if (__webpack_require__.nc) {
/******/ 			script.setAttribute("nonce", __webpack_require__.nc);
/******/ 		}
/******/ 		script.src = __webpack_require__.p + "" + chunkId + ".chunk.js";
/******/ 		var timeout = setTimeout(onScriptComplete, 120000);
/******/ 		script.onerror = script.onload = onScriptComplete;
/******/ 		function onScriptComplete() {
/******/ 			// avoid mem leaks in IE.
/******/ 			script.onerror = script.onload = null;
/******/ 			clearTimeout(timeout);
/******/ 			var chunk = installedChunks[chunkId];
/******/ 			if(chunk !== 0) {
/******/ 				if(chunk) chunk[1](new Error('Loading chunk ' + chunkId + ' failed.'));
/******/ 				installedChunks[chunkId] = undefined;
/******/ 			}
/******/ 		};

/******/ 		var promise = new Promise(function(resolve, reject) {
/******/ 			installedChunks[chunkId] = [resolve, reject];
/******/ 		});
/******/ 		installedChunks[chunkId][2] = promise;

/******/ 		head.appendChild(script);
/******/ 		return promise;
/******/ 	};

/******/ 	// expose the modules object (__webpack_modules__)
/******/ 	__webpack_require__.m = modules;

/******/ 	// expose the module cache
/******/ 	__webpack_require__.c = installedModules;

/******/ 	// identity function for calling harmony imports with the correct context
/******/ 	__webpack_require__.i = function(value) { return value; };

/******/ 	// define getter function for harmony exports
/******/ 	__webpack_require__.d = function(exports, name, getter) {
/******/ 		if(!__webpack_require__.o(exports, name)) {
/******/ 			Object.defineProperty(exports, name, {
/******/ 				configurable: false,
/******/ 				enumerable: true,
/******/ 				get: getter
/******/ 			});
/******/ 		}
/******/ 	};

/******/ 	// getDefaultExport function for compatibility with non-harmony modules
/******/ 	__webpack_require__.n = function(module) {
/******/ 		var getter = module && module.__esModule ?
/******/ 			function getDefault() { return module['default']; } :
/******/ 			function getModuleExports() { return module; };
/******/ 		__webpack_require__.d(getter, 'a', getter);
/******/ 		return getter;
/******/ 	};

/******/ 	// Object.prototype.hasOwnProperty.call
/******/ 	__webpack_require__.o = function(object, property) { return Object.prototype.hasOwnProperty.call(object, property); };

/******/ 	// __webpack_public_path__
/******/ 	__webpack_require__.p = "";

/******/ 	// on error function for async loading
/******/ 	__webpack_require__.oe = function(err) { console.error(err); throw err; };

/******/ 	// Load entry module and return exports
/******/ 	return __webpack_require__(__webpack_require__.s = 278);
/******/ })
/************************************************************************/
/******/ ([
/* 0 */
/***/ (function(module, exports) {

module.exports = polyfills_lib;

/***/ }),
/* 1 */,
/* 2 */,
/* 3 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(33);

/***/ }),
/* 4 */,
/* 5 */,
/* 6 */,
/* 7 */,
/* 8 */,
/* 9 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(651);

/***/ }),
/* 10 */,
/* 11 */,
/* 12 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(687);

/***/ }),
/* 13 */,
/* 14 */,
/* 15 */,
/* 16 */,
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(745);

/***/ }),
/* 19 */,
/* 20 */,
/* 21 */,
/* 22 */,
/* 23 */,
/* 24 */,
/* 25 */,
/* 26 */,
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(283);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(670);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(671);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(672);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(673);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(697);

/***/ }),
/* 40 */,
/* 41 */,
/* 42 */,
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/* 44 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(12);
__webpack_require__(151);
__webpack_require__(149);
__webpack_require__(155);
__webpack_require__(152);
__webpack_require__(158);
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__webpack_require__(148);
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__webpack_require__(153);
__webpack_require__(142);
__webpack_require__(144);
__webpack_require__(147);
__webpack_require__(146);
__webpack_require__(161);
__webpack_require__(34);
module.exports = __webpack_require__(3).Array;

/***/ }),
/* 45 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(162);
__webpack_require__(164);
__webpack_require__(163);
__webpack_require__(166);
__webpack_require__(165);
module.exports = Date;

/***/ }),
/* 46 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(167);
__webpack_require__(169);
__webpack_require__(168);
module.exports = __webpack_require__(3).Function;

/***/ }),
/* 47 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(9);
__webpack_require__(12);
__webpack_require__(18);
__webpack_require__(138);
module.exports = __webpack_require__(3).Map;

/***/ }),
/* 48 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(170);
__webpack_require__(171);
__webpack_require__(172);
__webpack_require__(173);
__webpack_require__(174);
__webpack_require__(175);
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__webpack_require__(180);
__webpack_require__(181);
__webpack_require__(182);
__webpack_require__(183);
__webpack_require__(184);
__webpack_require__(185);
__webpack_require__(186);
module.exports = __webpack_require__(3).Math;

/***/ }),
/* 49 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(187);
__webpack_require__(197);
__webpack_require__(198);
__webpack_require__(188);
__webpack_require__(189);
__webpack_require__(190);
__webpack_require__(191);
__webpack_require__(192);
__webpack_require__(193);
__webpack_require__(194);
__webpack_require__(195);
__webpack_require__(196);
module.exports = __webpack_require__(3).Number;

/***/ }),
/* 50 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(39);
__webpack_require__(200);
__webpack_require__(202);
__webpack_require__(201);
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__webpack_require__(199);
__webpack_require__(210);
__webpack_require__(214);
__webpack_require__(9);

module.exports = __webpack_require__(3).Object;

/***/ }),
/* 51 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(215);
module.exports = __webpack_require__(3).parseFloat;

/***/ }),
/* 52 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(216);
module.exports = __webpack_require__(3).parseInt;

/***/ }),
/* 53 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(217);
__webpack_require__(218);
__webpack_require__(219);
__webpack_require__(220);
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__webpack_require__(226);
__webpack_require__(227);
__webpack_require__(228);
__webpack_require__(230);
__webpack_require__(229);
module.exports = __webpack_require__(3).Reflect;

/***/ }),
/* 54 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(231);
__webpack_require__(232);
__webpack_require__(139);
__webpack_require__(35);
__webpack_require__(36);
__webpack_require__(37);
__webpack_require__(38);
module.exports = __webpack_require__(3).RegExp;

/***/ }),
/* 55 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(9);
__webpack_require__(12);
__webpack_require__(18);
__webpack_require__(140);
module.exports = __webpack_require__(3).Set;

/***/ }),
/* 56 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(242);
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__webpack_require__(12);
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__webpack_require__(35);
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__webpack_require__(37);
__webpack_require__(38);
module.exports = __webpack_require__(3).String;

/***/ }),
/* 57 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(39);
__webpack_require__(9);
module.exports = __webpack_require__(3).Symbol;

/***/ }),
/* 58 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(254);
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__webpack_require__(260);
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__webpack_require__(9);
module.exports = __webpack_require__(3);

/***/ }),
/* 59 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(9);
__webpack_require__(34);
__webpack_require__(141);
module.exports = __webpack_require__(3).WeakMap;

/***/ }),
/* 60 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(9);
__webpack_require__(18);
__webpack_require__(265);
module.exports = __webpack_require__(3).WeakSet;

/***/ }),
/* 61 */
/***/ (function(module, exports, __webpack_require__) {

__webpack_require__(266);
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__webpack_require__(269);
__webpack_require__(268);
__webpack_require__(271);
__webpack_require__(270);
__webpack_require__(272);
__webpack_require__(273);
__webpack_require__(274);
module.exports = __webpack_require__(3).Reflect;

/***/ }),
/* 62 */,
/* 63 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(447);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(448);

/***/ }),
/* 65 */,
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/* 137 */,
/* 138 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(409);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(410);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(411);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(412);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(578);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(579);

/***/ }),
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module.exports = (__webpack_require__(0))(580);

/***/ }),
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module.exports = (__webpack_require__(0))(581);

/***/ }),
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module.exports = (__webpack_require__(0))(582);

/***/ }),
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module.exports = (__webpack_require__(0))(583);

/***/ }),
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module.exports = (__webpack_require__(0))(584);

/***/ }),
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module.exports = (__webpack_require__(0))(585);

/***/ }),
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module.exports = (__webpack_require__(0))(586);

/***/ }),
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module.exports = (__webpack_require__(0))(587);

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module.exports = (__webpack_require__(0))(588);

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module.exports = (__webpack_require__(0))(589);

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module.exports = (__webpack_require__(0))(590);

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module.exports = (__webpack_require__(0))(591);

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module.exports = (__webpack_require__(0))(592);

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module.exports = (__webpack_require__(0))(593);

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module.exports = (__webpack_require__(0))(600);

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module.exports = (__webpack_require__(0))(601);

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module.exports = (__webpack_require__(0))(602);

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module.exports = (__webpack_require__(0))(603);

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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(604);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(605);

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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(606);

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module.exports = (__webpack_require__(0))(607);

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module.exports = (__webpack_require__(0))(616);

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module.exports = (__webpack_require__(0))(617);

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module.exports = (__webpack_require__(0))(618);

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module.exports = (__webpack_require__(0))(619);

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module.exports = (__webpack_require__(0))(620);

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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(621);

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/* 187 */
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/***/ (function(module, exports, __webpack_require__) {

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module.exports = (__webpack_require__(0))(627);

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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(628);

/***/ }),
/* 193 */
/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(629);

/***/ }),
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/***/ (function(module, exports, __webpack_require__) {

module.exports = (__webpack_require__(0))(630);

/***/ }),
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module.exports = (__webpack_require__(0))(636);

/***/ }),
/* 201 */
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Incredibly, even though Trump has made more than 5,000 false or misleading statements as president, major news organizations' social media feeds continue to inject his unadulterated lies into the political bloodstream without clearly informing readers that they are just that — lies.
On Wednesday, USA Today published a piece by Trump in which "almost every sentence contained a misleading statement or a falsehood," as Glenn Kessler put it. All these went initially uncorrected, and USA Today's feed featured multiple tweets spreading its falsehoods and distortions. We have seen this again and again.
That is, fake news authored by Trump himself.
There is little doubt that a deceiver as prolific and innovative as Trump grasps — whether instinctively or consciously — that those getting news from social media and on mobile devices often read no further than headlines or tweets, and that the transmitting out of disinformation that gets amplified in headlines and news feeds helps him exploit this facet of the shifting information landscape.
"The importance of headlines is arguably even greater now in the social media era, because a lot of people are in passive consumption mode," Craig Silverman, the media editor at BuzzFeed News, told me. BuzzFeed came of age in the Internet area, so has perhaps been quicker than others to grasp the disinformational danger this poses.
This is a crucial insight, and while things have gotten better in recent months, the problem remains one that plenty of traditional journalists and news organizations still refuse to take seriously enough. You constantly see headlines on news organizations' websites that blare forth a politician's false, dubious or unsupported claims without informing readers that those claims are, well, false or dubious or unsupported. Often it requires reading deep into a story to discover a corrective, if there is a corrective at all.
Early in the Trump presidency, media critic Jay Rosen wrote a pair of prescient essays arguing that Trump's nonstop falsehoods were part of something much bigger — a concerted and deliberate assault by Trump and his allies on the media's core institutional role in our democracy, one aided and abetted by shifting information technologies. In response, Rosen argued, media figures must commit to a new public mindset that mounts a concerted defense of the news media's core liberal democratic values, in part by treating the totality of Trump's lies as the broader threat that they really represent.
American journalism has confronted moments like this before. In the late 1960s and early 1970s, the profession was tested in then-new ways by a confluence of cultural and political changes, including the growth of the federal government and mass media; the increasing transparency of Congress via innovations such as the Freedom of Information Act; and the massive official deception around the Watergate scandal and the Vietnam War.
As media scholar Michael Schudson has recounted, journalists and news organizations adapted by becoming more probing and analytical, and by asserting themselves more aggressively toward powerful figures. These changes, Schudson noted, brought a "new skepticism and critical instinct to journalism," which enabled the profession to evolve along with changes in American society and political culture.


text:
Villerest és un municipi francès situat al departament del Loira i a la regió d'Alvèrnia-Roine-Alps. L'any 2007 tenia 4.414 habitants.

Demografia

Població
El 2007 la població de fet de Villerest era de 4.414 persones. Hi havia 1.656 famílies de les quals 286 eren unipersonals (103 homes vivint sols i 183 dones vivint soles), 645 parelles sense fills, 649 parelles amb fills i 76 famílies monoparentals amb fills.

La població ha evolucionat segons el següent gràfic:

Habitants censats

Habitatges
El 2007 hi havia 1.803 habitatges, 1.689 eren l'habitatge principal de la família, 24 eren segones residències i 89 estaven desocupats. 1.695 eren cases i 104 eren apartaments. Dels 1.689 habitatges principals, 1.457 estaven ocupats pels seus propietaris, 213 estaven llogats i ocupats pels llogaters i 20 estaven cedits a títol gratuït; 3 tenien una cambra, 36 en tenien dues, 115 en tenien tres, 510 en tenien quatre i 1.025 en tenien cinc o més. 1.391 habitatges disposaven pel capbaix d'una plaça de pàrquing. A 627 habitatges hi havia un automòbil i a 981 n'hi havia dos o més.

Piràmide de població
La piràmide de població per edats i sexe el 2009 era:

Economia
El 2007 la població en edat de treballar era de 2.925 persones, 2.037 eren actives i 888 eren inactives. De les 2.037 persones actives 1.886 estaven ocupades (1.000 homes i 886 dones) i 152 estaven aturades (66 homes i 86 dones). De les 888 persones inactives 411 estaven jubilades, 263 estaven estudiant i 214 estaven classificades com a «altres inactius».

Ingressos
El 2009 a Villerest hi havia 1.711 unitats fiscals que integraven 4.591,5 persones, la mediana anual d'ingressos fiscals per persona era de 19.729 €.

Activitats econòmiques
Dels 139 establiments que hi havia el 2007, 8 eren d'empreses extractives, 1 d'una empresa alimentària, 1 d'una empresa de fabricació de material elèctric, 8 d'empreses de fabricació d'altres productes industrials, 16 d'empreses de construcció, 32 d'empreses de comerç i reparació d'automòbils, 8 d'empreses de transport, 14 d'empreses d'hostatgeria i restauració, 9 d'empreses financeres, 3 d'empreses immobiliàries, 15 d'empreses de serveis, 14 d'entitats de l'administració pública i 10 d'empreses classificades com a «altres activitats de serveis».

Dels 26 establiments de servei als particulars que hi havia el 2009, 1 era una oficina de correu, 1 una oficina bancària, 4 tallers de reparació d'automòbils i de material agrícola, 3 paletes, 2 guixaires pintors, 3 lampisteries, 3 perruqueries, 8 restaurants i 1 agència immobiliària.

Dels 5 establiments comercials que hi havia el 2009, 1 era un supermercat, 1 una fleca, 1 una botiga de roba, 1 una botiga d'equipament de la llar i 1 una botiga de material esportiu.

L'any 2000 a Villerest hi havia 18 explotacions agrícoles que ocupaven un total de 246 hectàrees.

Equipaments sanitaris i escolars
Els 2 equipaments sanitaris que hi havia el 2009 eren farmàcies.

El 2009 hi havia 2 escoles maternals i 2 escoles elementals.

Poblacions més properes
El següent diagrama mostra les poblacions més properes.

Referències

 Résumé statistique Fitxa resum de dades estadístiques de Villerest a l'INSEE.
 Évolution et structure de la population Fitxa amb el detall de dades de Villerest a l'INSEE
 France par commune Dades detallades de tots els municipis de França accessibles a partir del mapa.

Municipis del Loira

redpajama_set_name: RedPajamaWikipedia


Fallenwood is the story of a girl named Ash who, running away after the death of her stepfather, finds her way to a strange and magical world. But the world she now finds herself in - a world that was once called Terra Illumina but now is known as "Fallenwood" - is a world threatening to tear itself apart. Magic is the life force of Fallenwood, and if it keeps being used up, everything will die. But magic is a weapon, and weapons are owned for the sake of power. Now Ash must find a way to destroy the Great Crystal - the catalyst through which all magic in Fallenwood is channelled - and meanwhile, the kingdoms are going to war. Can she save Fallenwood before it's too late?


What do you need to know in order to be happy? Successful? Is it beating the competition to learn breaking news before anyone else? Obsession with a topic or idea leader? Wanting to be connected to important ideas? Not wanting to be blind-sided by missing information? Or just too busy to throw anything away? When should you unplug?
Introduction: The Information Audit: Why Are You Spending Your Time Immersed?
Improve the quality of the resources you use.
Free more time for acting on existing data.


Becky Lary graduated from LSUS with a Bachelor's Degree in Elementary Education. She has taught in Caddo Parish since 1995, with most of those years teaching first grade. Mrs. Lary's became an Eden Gardens first grade teacher in 2005.


text:
ARRL Board of Directors to Elect New President, Officers at January Meeting
TAGS: 16th president, 2-year terms, annual meeting, arrl board, ARRL Chief Executive, ARRL Chief Operating, ARRL First Vice, arrl headquarters, ARRL President Kay, arrl section manager, Atlantic Division Vice, CEO Search Committee, chief executive officer, craigie, eastern pennsylvania, Executive Vice President, finance committee, new CEO, Officer David Sumner, Officer Harold Kramer
The ARRL Board of Directors' annual meeting in mid-January will mark the beginning of a changing of the guard for the League. After serving three 2-year terms, ARRL President Kay Craigie, N3KN, of Blacksburg, Virginia, is stepping aside, and the Board will choose her successor — and the League's 16th president — when it convenes on January 15. The Board also will elect other officers, as well as vice presidents, Executive Committee members, and ARRL Foundation directors.
A former college instructor, Craigie was licensed in 1983. She served previously as ARRL Section Manager for Eastern Pennsylvania, Atlantic Division Vice Director and Director, and ARRL First Vice President. As President, Craigie presided during the League's Centennial and transition into its second century.
The annual meeting also will be the last for ARRL Chief Executive Officer David Sumner, K1ZZ, and for ARRL Chief Operating Officer Harold Kramer, WJ1B. Both are retiring this year. Kramer will depart at the end of February. Sumner has targeted May 1 as his last day, and he plans to work with the new CEO to ensure a smooth transition. During the annual meeting, the Board will receive the report of the CEO Search Committee, which is expected to include a recommendation for Sumner's successor. The Board initiated its CEO search last July. The COO position will remain vacant until the new CEO is in place.
By the time he steps down, Sumner will have been on the ARRL Headquarters full-time staff for 44 years. He was named Secretary and General Manager in 1982, with a change in title to Executive Vice President in 1985, and the additional title of Chief Executive Officer in 2001 (the title of Executive Vice President was phased out in 2011).
The Board of Directors also will receive the report of the Strategic Planning Working Group, which has been working on a revised Strategic Plan to guide the League in the coming years. In addition the Administration & Finance Committee will ask the Board to ratify the operational budget plan for 2016-17.
The ARRL Board of Directors' annual meeting will take place Friday and Saturday, January 15 and 16, in Windsor, Connecticut.
News & Features >> News
ARRL News: Coronavirus COVID-19
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\section{Introduction}
Observations of active galactic nuclei (AGN) clearly show
 different types of emission lines in their
spectra. Depending on the width of the emitted lines,
they are classified as  narrow lines,
with full width half maximum (FWHM) $\sim$ 500 km s$^{-1}$,
or broad lines, with
FWHM $\gtrsim$ 2000 km s$^{-1}$.
This implies two different regions of line formation, i.e, narrow
line region (NLR) and the broad line region (BLR)
respectively.
Although the physical
conditions of these regions are quite well
understood
\citep{davidson1972,krolik1981,netzer1990,pier1995,dopita2002,groves2004a,
groves2004b,stern2014,baskin2014,czerny2011,czerny2015,stern2016},
there are still several issues to be explored. One of those problem
is the significant suppression of
the line emission in a region between the BLR and NLR in most AGN
\citep{osterbrock2006, boroson1992}. A leading explanation for this feature
is the dust suppression introduced by \citet[hereafter NL93]{netzer1993}.
On the other hand,  recent observations of several objects
indicate the existence of
an intermediate line emission region (ILR), between the BLR
and NLR, which produces emission lines
with velocity FWHM $\sim$ 700 - 1200 km s$^{-1}$.
Using the statistical investigations of broad UV-lines in QSOs,
\citet{brotherton1994} discussed the ILR as an inner extension of the NLR.
\citet{mason1996} found  evidence for an ILR with velocity
FWHM $\sim$ 1000 km s$^{-1}$ which produces a
significant amount of both permitted and
forbidden line fluxes in NLSy1 RE~J1034+396.  For the Sy1
NGC 4151, \citet{crenshaw2007} identified a
line emission component with  width FWHM $=$ 1170 km s$^{-1}$, most probably
originating between the BLR and NLR. Detailed spectral analysis of large number of
{\it SDSS} sources have revealed the presence of intermediate component of
line emission with velocity width in between that of broad and narrow components \citep{hu2008a,hu2008b,zhu2009}.
Additionally, \citet{crenshaw2009}
detected  ILR emission with width of 680 km s$^{-1}$ in the historically
low state spectrum of NGC 5548 obtained with
the Space Telescope Imaging Spectrograph on the
{\it Hubble Space Telescope}. Using the {\it HST/ FOS} spectra of quasar OI 287,  \citet{li2015} reported
 the detection of intermediate width emission lines originating at
 a distance of $\sim$ 2.9 pc from the central black hole.
The question remains unanswered, is there any
separation between gas responsible for broad
and narrow line emission in different types of
AGN? What is the physical mechanism
leading to the existence of this gap in some source, and
why the gap is not observed in all of them?

Photoionization calculations provide a powerful
tool to model the line emission
from gas clouds powered by the
continuum radiation from the nucleus.
Detailed analysis  has  shown that BLR clouds
are denser and located closer to the AGN center,
while the NLR clouds have lower density and are more distant
\citep[see for details][]{osterbrock2006,netzer1990}.
Nevertheless, the lack of significant line emission from
the intermediate zone between the BLR and NLR
is not naturally explained by photoionization models.

The presence of dust complicates the physics by introducing
additional processes
\citep[and references therein]{ferland1979,baldwin1991,vanhoof2004}
in the radiation-matter interactions
which has to be treated properly in  simulations of
the gas emission.
Observations have shown the existences
of dust in the NLR for almost all types of AGN
\citep[]{derobertis1984,ferland1986,wills1993}.
However, it has been argued that the BLR clouds are devoid of dust
since there is a lack of depletion of refractory elements in the gaseous phase \citep{gaskell1981}.
Usually, it is believed that, the radiation energy is so high
in BLR, that the dust if present sublimes and no longer
survives there \citep{czerny2011}.
Reverberation mapping studies show that the BLR clouds are located at a distance smaller by a factor 4 to 5 than the hot dust emission
\citep{suganuma2006,koshida2014}.
On the other hand, \citet{nenkova2008} has shown that the  closest region where dust can survive in the full radiation field is the face
of the dusty torus, located approximately at 0.4 pc for AGN of typical luminosity (see their Eq.~1).
While Eq.~1 of \citet{nenkova2008} gives the smallest radius
 at which the dust absorption coefficient reflects the full grain mixture, the largest
grains survive to closer radii, where they are presumably detected
by the reverberation measurements.

The observed apparent gap in the line emission region between BLR and NLR was explained
by the dust content in NLR clouds by NL93.
The authors  calculated  emission from
a continuous radial distribution of clouds
extending from the BLR to the NLR, using the numerical photoionization code
{\sc ION} \citep{rees1989}.
Their assumption was that the dust is present in NLR
but sublimes in a higher ionization region,
around the BLR. The authors have shown that the reduced line
emission vs radius is a result of the dust extinction of
ionizing radiation as well as the dust destruction of
the line photons. The dust absorption
becomes more efficient with decreasing  radial
distance from the nucleus, and gives rise to an empty intermediate
region, where gas is present but the line emission is heavily suppressed.
The dust fully sublimates at smaller radii,
and  line emission increases
dramatically, by about an order of magnitude, giving rise to the BLR.
NL93 successfully demonstrated the apparent gap in the line emission vs radius,
although their result was obtained for a
particular spectral energy distribution (SED) typical for Sy1 AGN
\citep{Mathews1987}, and for a specific value of the density
$n_{\rm H} = 10^{9.4}$ cm$^{-3}$ at the sublimation radius at $\sim~0.1$ pc.

The aim of this paper is to explain the disappearance of an
apparent gap in line emission seen for some sources
within the framework of NL93 model.
We use the photoionization code {\sc cloudy}, version 13.03
\citep[][]{ferland2013} to determine line luminosities
for different shapes
of the incident radiation representative for various sub-classes
of AGN, as measured from recent observations:
Sy1.5 galaxy Mrk 509 \citep{Kaastra2011},
Sy1 galaxy NGC 5548 \citep{Mehdipour2015}, and
NLSy1 galaxy PMN J0948+0022 \citep{ammando2015}.
In addition, we also use a flexible
parametric shape of SED as a
Band function \citep{band1993}.
All our results presented below focus on the five major emission
lines usually detected in those objects:
H${\beta}$ ${\lambda}$4861.36 \AA, He~II ${\lambda}$1640.00 \AA,
Mg~II ${\lambda}$2798.0 \AA, C~III] ${\lambda}$1909.00 \AA
~and [O~III] ${\lambda}$5006.84 \AA.

We show, that the various shapes of SED used in our computations
with the model parameters taken from NL93 do not remove apparent gap in the
line emission vs radius. For lines considered by us, we always obtain
apparent gap similar to the result of NL93.
Therefore, the observed properties of ILR cannot be explained only by considering the
different shapes of radiation illuminating the gas and dust in our simulations.
However, increasing the gas density at the sublimation
radius yields to the continuous line
emission vs radius and fully explains the observed emission from the ILR.

The structure of this paper is as follows:
Section~\ref{sec:parameters} describes the parameter
set up of our photoionization simulations.
In Section~\ref{sec:sed_dependence}, we
present the major line luminosity radial profiles for
various SEDs. The same line emission vs radius, but
for different gas densities, are presented
in Section~\ref{sec:density_dependence}.
Finally, the discussion and conclusions of our work are described
in Sections~\ref{sec:disc}~and~\ref{sec:con}.

\section{The model and its parameters}
\label{sec:parameters}

We consider the continuous distribution of optically thick spherical clouds
above an accretion disk,
placed at different radial distances extending
from the BLR ($\sim 10^{-2}$ pc) to the NLR ($\sim 10^{3}$ pc).
Each cloud at radial distance $r$ from the nucleus represents the
gas in the emission region described by the parameters:
hydrogen number density, $n_{\rm H}$ [cm$^{-3}$], dimensionless ionization
parameter, $U$, total hydrogen column density, $N_{\rm H}$ [cm$^{-2}$],
and the chemical abundances.  We note that, in the recent years, there is a
growing evidence that the emitting and absorbing clouds are radiation pressure confined,
and thus the total
(radiation+ gas) pressure inside the cloud is constant with stratification in matter density
\citep{pier1995,dopita2002,groves2004a,groves2004b,rozanska2006,stern2014,baskin2014,adhikari2015,stern2016}. However, we have checked the assumption that each cloud is in pressure equilibrium does not change the main conclusion of our paper, therefore here we consider
the constant density clouds to keep the consistency with the NL93 formalism.
The ionization parameter is defined as the ratio of the number of hydrogen-ionizing
photons, $Q_{\rm H}$ [s$^{-1}$], to the gas density of
the cloud \citep{osterbrock2006}
\begin{equation}
\label{eq:U}
U=\frac{Q_{\rm H}}{4\pi r^{2}n_{\rm H}~ c}
\end{equation}
where $c$ is the velocity of light.

These clouds are illuminated by the radiation of different spectral shapes
shown in Fig.~\ref{fig:seds}. To consider various types of AGN we used the
SED of the Sy1.5 galaxy Mrk 509 as measured in
multi-wavelength observation campaigns \citep{Kaastra2011} and
the Sy1 galaxy NGC 5548 \citep{Mehdipour2015}.
The SED of Mrk 509 is dominated by  soft X-ray photons below 1 keV,
whereas the SED of NGC 5548 is dominated by harder photons above 2 keV.
To represent the SED of a NLSy1
we use the galaxy PMN J0948+0022 \citep{ammando2015}, shown as the magenta dashed line.
The NLSy1 galaxy PMN J0948+0022 SED has no pronounced emission around $\sim$ 0.1 keV,
rather it has an  excess of harder photons.
We also consider the spectral shape produced with the Band
function $f(E)$ \citep{band1993} as another typical  active galaxy.
Band function combines two power laws smoothly
and provides the possibility of creating  different shapes of spectra
by allowing to change the parameters in the following expression:
\begin{equation}
\label{eq:bandf}
\begin{split}
f(E) & =  A\Big[\frac {E}{100}\Big]^{\alpha}~e^{\Big[\frac{-2(E+\alpha)}{E_{\rm p}}\Big]},~~~ {\rm for}~ E<\frac{(\alpha-\beta)E_{\rm p}}{(2+\beta)}\\
 & = A\Big[\frac{(\alpha-\beta)E_{\rm p}}{100(2+\alpha)}\Big]^{(\alpha-\beta)}\Big(\frac{E}{100}\Big)^{\beta}e^{(\beta-\alpha)},\\
 & ~~~~{\rm for}~ E\geq\frac{(\alpha-\beta)E_{\rm p}}{(2+\beta)}\\
\end{split}
\end{equation}
where $\alpha$ and $\beta$ are the slopes of the first and
second power law respectively. $E_{\rm p}$ is the peak energy, where the
two power laws combine smoothly.
For producing the Band SED shape, we choose the slope
of the first power law $\alpha=0.51$ which cuts off
exponentially at $13.3$ eV and the second power law with slope $\beta=-1.5$.
These SEDs are chosen for two reasons:
(i) they are recently constrained by combining the data
from multi-wavelength observations (except the Band SED)
and (ii) they represent different possible SEDs that
an AGN can have in general.

 \begin{figure}[h]
\includegraphics[width=0.48\textwidth]{seds_report_small.eps}
\caption{\small Shapes of the broad band spectra used in our photoionization calculations.
All SEDs are normalised to the
$ L = 10\rm {^{45}~erg~s^{-1}}$ and represent the radiation illuminating
the cloud at $r$ = 0.1 pc.
The dashed line shows Mrk 509, while the
solid line describes NGC 5548.  The SED of the
NLSy1  PMN J0948+0022 is presented as the
dashed dotted line, and the SED produced with the Band
function is shown by the dotted line.
See Section~\ref{sec:parameters} for parameters and references.}
\label{fig:seds}
\end{figure}

For deriving the luminosities
of the emission lines corresponding to each individual
portion of gas at the given distance,
we make simulations with the photoionization {\sc cloudy} code (version  c13.03)
\citep{ferland2013}.
We use the {\it luminosity case} in {\sc cloudy} with an assumed source luminosity of
$L=\rm~10^{45} ~ erg~s^{-1}$. Thus, the ionization parameter $U$
for each cloud is computed by the code itself.
The shape of the continuum is given by points using the
{\it interpolate} command (for details see {\sc cloudy}
documentation files\footnote{http://www.nublado.org/}).
We employed the profiles of the cloud parameters as
a function of $r$ as described by NL93:
\begin{equation}
\label{eq:params}
n_{\rm H}\propto r^{-3/2},~~~ N_{\rm H}\propto r^{-1}.
\end{equation}

To investigate  the effect of the SED on the resulting
line luminosities, the normalization of parameters in
Eq.~\ref{eq:params} is  chosen after NL93 that at $r=0.1$ pc,
$n_{\rm H}=\rm ~10^{9.4} ~ cm^{-3}$ and $N_{\rm H}=\rm~10^{23.4}~cm^{-2}$.
With this choice of normalization, the values of $n_{\rm H}$ and
$N_{\rm H}$ of the cloud at the closest distance, $r$ = 10$^{-2}$ pc, are
${\rm 10^{10.9} ~ cm^{-3}}$ and ${\rm 10^{24.4}~cm^{-2}}$ respectively.
The most distant cloud, at $r$ =10$^{3}$ pc, has values of
${\rm 10^{3.4} ~ cm^{-3}}$ and  ${\rm 10^{19.4}~cm^{-2}}$ respectively.
As justified in NL93,
these numbers are reasonable for simulating the BLR-NLR system of an
AGN with a bolometric luminosity of $10^{45}$~ erg~s$^{-1}$.
The choice of the sublimation radius
at $0.1$ pc is not obvious, since it depends on the size and the grains composition \citep{netzer2013}.
However, for the purpose of understanding
the global properties of the line emission vs radius this
assumption is reasonable and was also used by NL93.

We used the {\sc cloudy} default solar composition
for clouds located at  $r\leq$ 0.1 $\rm pc$ and for
more distant clouds at $r>$ 0.1 $\rm pc$
the interstellar medium (ISM) composition with
dust grains is used. This includes the graphite and silicate
component appropriate for the ISM of our galaxy
and is fully taken into account by the {\sc cloudy} code.

To investigate the role of the cloud density on our results, we change the normalization
 to give different values of the gas density number at the sublimation radius.
We consider the following four different number densities:
$n_{\rm H}=\rm~10^7, 10^{10}, 10^{11}, 10^{11.5} ~ cm^{-3}$ at $r=0.1$~pc
while keeping the other parameters same.

\section{Line emission vs radius for various SEDs}
\label{sec:sed_dependence}

In this section we set the density normalization as in NL93, so that
$n_{\rm {H}}$=10$^{9.4}$ cm$^{-3}$ at $r$ = 0.1 pc.
The emission-line luminosity radial
profiles for the lines: H${\beta}$ (red circles), He~II
(green triangles down), Mg~II (cyan triangles up), C~III] (magenta pluses)
and [O~III] (blue crosses) are shown in
Fig.~\ref{fig:line_profile}.
The upper panels of the figure show the line
luminosities for Mrk 509 (left) and NGC 5548 (right). In the
lower panels, results for PMN J0948+0022 (left) and Band function
(right) are presented.

\begin{figure}
\hspace{-0.6cm}
\includegraphics[width=0.53\textwidth]{net_laor_profile_new.eps}
\caption{\small The line emission vs radius for various lines:
H${\beta}$ (red circles), He~II (green triangles down), [O~III] (blue crosses),
Mg~II (cyan triangles up) and C~III] (magenta pluses) shown as a function of radius
from the illuminating source. For all panels $n_{\rm H}=10^{9.4}$ cm$^{-3}$
at $r$ = 0.1 pc.  Total dust emission (magenta continuous line) and
the total gas emission (black dashed line) are shown for clarity.
Upper left panel presents the results for spectral shapes of Mrk~509, upper right panel
- NGC 5548, lower left - NLSy1 PMN J0948+0022, and lower right panel
- Band function.}
\label{fig:line_profile}
\end{figure}

The nature of the line emission vs radius is similar for
Mrk 509, NGC 5548, and the Band function, independently of the shape
of the illuminating radiation.
For all the  considered lines, the radial emission profiles
display the strong suppression (by a factor of $\sim$ few
to a few orders of magnitude)
of the line luminosity in a region
close to the sublimation radius. The suppression of the emission can
also be noticed in the profile of the total gas emission
(black dashed lines in the figure). These results are in agreement with the
result of NL93 performed for only the one standard AGN SED \citet{Mathews1987} used by those authors.
However, the radial luminosity profile of the He~II line is only
weakly suppressed by the factor of $\sim$ 3
with the inclusion of dust. This is different from the case of NL93,
where the He~II emission goes down by $\sim$ an order of magnitude.

Considerably
different radial emission profile
for the semi-forbidden line C~III] and forbidden line [O~III] is obtained in case
of NLSy1 PMN J0948+0022 SED.
The C~III] line luminosity decreases steeply with increasing radius
showing a different behaviour from the other SEDs, where
it increases in a region between 0.1$<r<$10 pc.
As can be seen from the Fig.~\ref{fig:line_profile} (lower left panel),
the [O~III] emission is not significant in a region corresponding to the
NLR ($r~\sim$10~-~100 pc), which is different from the other SEDs
where an excess of [O~III] emission is seen at those distances.
Interestingly, this result is consistent with the SDSS spectrum of
PMN J0948+0022, where  [O~III] emission is not present
\citep[][see their Fig.~2, lower panel]{tanaka2014}.
Finally, our model shows that He~II emission in this object is not
significantly affected by the presence of dust.  Rather, it is fairly constant
close to 0.1 pc and decreases slowly as a function of radial distance.
The differences in line emission of C~III], [O~III] and He~II
from the other SEDs considered in our study are
connected with the fact that the PMN J0948+0022 SED
has fewer photons in the extreme UV and soft X-ray band. This significantly smaller number
of hydrogen ionizing photons causes the drastic drop, by two orders of magnitude,
in lines emitted in the lower density dusty medium on the larger radii.

Despite these differences, the effect of dust on the line suppression is
clearly visible in the case of PMN J0948+0022, and it is the strongest
for the high luminosity H${\beta}$ and Mg~II lines.
The general conclusion is that for  gas with physical
conditions and parameters
given by NL93, the apparent gap in the line emission cannot be removed
by changing the shape of illuminating continuum.
The differences in the [O~III], C~III] and He~II radial luminosity profiles
for NLSy1 SED are not sufficient to explain the origin of the
ILR.

\section{Role of the gas density}
\label{sec:density_dependence}

\begin{figure}
\hspace{-0.6cm}
\includegraphics[width=0.53\textwidth]{net_laor_profile_hden_new.eps}
\caption{\small
Same as in Fig.~\ref{fig:line_profile}, but density $n_{\rm H}=\rm ~10^{11.5} ~ cm^{-3}$ at the sublimation radius, $r$=0.1 pc.}
\label{fig:line_profile_hd}
\end{figure}

High local densities in the BLR ($n_{\rm H}$ $\sim 10^{11} - 10^{11.5}$ cm$^{-3}$)
have been deduced from the study of  UV Fe~II emission of an extreme NLSy1 object, I Zw 1
\citep{bruhweiler2008}, and in the quasars:  LBQS 2113-4538 \citep{hryniewicz2014}, CTS C30.10
\citep{modzelewska2014}, and HE 0435-4312 \citep{sredzinska2016}.
Additionally, a density  of $10^{10.25}$ cm$^{-3}$ was found from the study of UV
intrinsic absorbers of two NLSy1 galaxies  \citep{karen2004}.
Finally, from photoionization calculations, \citet{rozanska2014} found the density of
an intrinsic absorbing cloud in the bright quasar HS 1603 + 3820 to be
of the order of $n_{\rm H}$ $\sim 10^{10} - 10^{12}$ cm$^{-3}$.
On the basis of those results, we increased the normalization of the gas density
at  $r$=0.1 pc, to be $n_{\rm H}=\rm~10^{11.5} ~ cm^{-3}$ in our model.
Note, that the ionization parameter changes inversely with $n_{H}$
as given in Eq.~\ref{eq:U}, but all other parameters have the same values
as described in Sec.~\ref{sec:parameters}.

The resulting emission profiles of the five major lines are shown
in Fig.~\ref{fig:line_profile_hd} for the  four SEDs.
The meaning of lines and points is exactly the same as in Fig.~\ref{fig:line_profile}.
The H${\beta}$,
He~II, and C~III] emission lines behave differently from the
 lower density normalization case.
The presence of dust does not suppress  H${\beta}$ and C~III]
line emission, rather it is enhanced by the factor of
$\sim$ 1.5 at $0.1<r<0.3$ pc, in the case of the Mrk~509, NGC~5548 and  Band
function SEDs. For the SED of NLSy1 PMN J0948+0022 C~III] emission increases
by the factor of $\sim$ 3 at $0.1<r<0.3$ pc, whereas H${\beta}$ emission
decreases slightly with the distance, but there is no large jump
at the sublimation radius, as was found in the lower density
case. Only the Mg~II line displays a jump at 0.1~pc, but it is much less prominent than in
the lower density case. In all other cases we observe the lack of the line suppression
for all shapes of SED.

Our result clearly shows that the strong
suppression in the line emission  at the sublimation radius
for lower density normalization, disappears at the higher density.
Therefore, intermediate line emission can be produced at radial distances
$r~\sim$ 0.1 - 1 pc. Note, that the gas emission
also does not display any jump for high density case.
The strong ILR emission found by
\citep{mason1996,crenshaw2007,crenshaw2009}, can be produced
if the clouds are two orders of magnitude denser than those
considered by NL93. Our results corroborate with the speculation made
by \citet{landt2014}, where they discuss the possible role of high density gas for the production of smooth BLR.
Furthermore, if the ILR is located at distances predicted by our model, we can estimate
the expected reverberation mapping lag. Within the framework of our model, the ILR lag would be of the order of 100-1000 light-days.

\begin{figure}
\hspace{-0.6cm}
\includegraphics[width=0.53\textwidth]{varden.eps}
\caption{\small
The line emission vs radius for different densities:
$ n_{\rm H}=10^{7.0}$~(red~circles),~ $10^{9.4}$~(green~triangles~down),
$10^{10.0}$~(blue~triangles~up),~ $10^{11.0}$~(magenta~hexagons)
and ~ $10^{11.5}$ (black~pentagons) cm$^{-3}$ at $r=0.1$ pc.
The left and right panels show the case of the Sy1.5 Mrk 509
and NLSy1 PMN J0948+0022 SEDs respectively.
Five major lines: H${\beta}$, He~II, [O~III], Mg~II and C~III] are presented from top to
bottom. The detection limit on line luminosity is
shown by horizontal black dashed line (see text for details).}
\label{fig:varden}
\end{figure}

The physical reason for the density dependence is connected with the value of the column density
at which the ionization front is located. Below, we explain this in the example of hydrogen
H${\beta}$ line. Let us assume simple ground-state hydrogen photoionization, and set the ionization balance equation
\begin{equation}
n_{\rm p}~n_{\rm e}~ l~ \alpha_{\rm B}(T) = \phi_{\rm H}.
\end{equation}
\citep{osterbrock2006}.
The first two terms are the proton and electron density in the H$^+$ layer of the cloud,
$l$~[cm] is the thickness of the H$^+$ layer, and $\alpha_{\rm B}(T)$~[cm$^{3}$~s$^{-1}$] is the
Case B recombination coefficient. The physical interpretation is that the flux of hydrogen-ionizing
photons incident on the cloud, $\phi_{\rm H}$~[cm$^{-2}$~s$^{-1}$], equals the number of
hydrogen recombinations that occur over the thickness $l$.

The hydrogen column density across H$^+$ layer is then
\begin{equation}
\label{eq:h+col}
N_{\rm H^+} \equiv n_p l =  \frac{\phi_{\rm H}}{n_{\rm e} \alpha_{\rm B}(T)} = U c~\alpha_{\rm B}(T)^{-1} .
\end{equation}
The gas column density $N_{\rm H^+}$, and resulting line and continuum optical depths,
all scale with the ionization parameter. At very high values of $U$, whole cloud is ionized,
and the line emission comes from the whole volume, in this case limited
by the fixed adopted total hydrogen column, $N_{\rm H}$.
As the cloud density increases, the ionization
parameter decreases, ionization front forms, and the cloud consist of two zones.
The line emission comes from the first zone, and only the dust in this zone competes
with the gas for the photons. The high-density clouds
studied here have smaller column densities and optical
depths of H$^+$ layer, since ionization parameter is lower.
This is clearly demonstrated in Fig.~\ref{fig:ion_density}, which shows that
the H$^+$ - H$^0$ ionization front moves towards smaller cloud
thickness with increasing number density of the cloud.
For smaller values of $U$, the dust absorption decreases,
so there is less suppression of the emission due to the
presence of dust. In other words, the less dense clouds
have much larger thickness of H+ layer, larger dust column density in the
zone with abundant photons, and therefore the
dust absorption is significant.

Eq.~\ref{eq:h+col} can be used for the quantitative estimation of threshold U,
below which the gas opacity for incident photons dominates over opacity of dust.
Taking recombination coefficient $\alpha_{\rm B}~(\rm at ~10^{4}~ K)~= $~ 2.6$\times 10^{-13}$ cm$^{3}$~s$^{-1}$, gives the column density:
$N_{\rm H^+}~\sim~$ 10$^{23}~U$. Therefore, the dust optical depth for UV photons is
$\tau_{\rm dust} \cong N_{\rm H^+}/10^{21}$ = 100 $U$ \citep[for details see][]{guver2009}.
For $U$=0.1,
$\tau_{\rm dust}$ =10 at the edge of the H$^{+}$ region.
This implies that the width of the H$^{+}$ layer where gas actively
absorbs and emits is only 1/10 of the
total layer.
In other words, increasing the density by the
factor $>$ 10 would mean $U~<$ 0.01 which implies $\tau_{\rm dust}$ $<$ 1.
This means that the gas opacity always dominates for higher densities  and
it does not matter if the gas is dusty or not, and therefore no
suppression of the line emission is physically possible.

 It is worth to mention the conclusion of
\citet{ferland1983}, saying that for low ionization nuclear emission line region (LINERs), if
the line emission comes from the photoionised gas, the
 $U$ is $\leq~\rm 10^{-3}$. This is less than the threshold $U$
corresponding to higher density (10$^{11.5}$ cm$^{-3}$) implied by our result,
where the gas opacity is always dominant over the opacity of dust. So, our result
clearly indicates that LINERs should also exhibit the ILR. We note that the
presence of ILR in LINERs is also discussed by \citet{balmaverde2016}
where they analysed 33 LINERs (bona fide AGN) and Seyfert galaxies from
optical  spectroscopic  Palomar  survey  observed  by  {\it HST/STIS}.
However, the density of the outer portions of ILR claimed by those authors is about three orders
of magnitude less (i.e., 10$^4$-10$^5$ cm$^{-3}$) than what our model predicts. Most probably this
is due to the fact that LINERs are much fainter than objects considered in this paper.

\begin{figure}
\hspace{-0.6cm}
\includegraphics[width=0.56\textwidth]{ion_density_mrk509_ii.eps}
\caption{\small Ionized (H$^{+}$) and neutral (H$^{0}$) hydrogen densities
relative to the total cloud denesity $n_{\rm H}$, as a function of
column density across the cloud  illuminated by SED of Mrk 509.
The left and right panels show the ion densities for $n_{\rm H}= 10^{11.5}$ and $10^{9.4}$
cm$^{-3}$ at $r = 0.1$ pc respectively. Values of $n_{\rm H}$ change
with $r$ as Eq.~\ref{eq:params}, and are given in each panel together with the
cloud location.}
\label{fig:ion_density}
\end{figure}
\section{Discussion}
\label{sec:disc}

\subsection{Individual line behaviour}

Beside the general trend presented
above, in some cases we note exceptional line behaviour.
For instance, Mg~II (cyan triangles up in Figs.~\ref{fig:line_profile},
and \ref{fig:line_profile_hd}) line emissivity does not depend
on the shape of the SED. All SEDs considered by us
produce the emissivity jump at the sublimation radius, but this jump is
two orders of magnitude higher when the cloud  density is lower,
due to physical reason given above, but for the case of magnesium ionization front.

The density influence on the suppression of line luminosity jump at the sublimation
radius is best seen in case of H${\beta}$. For all continuum shapes the
strong jump in emission (order of magnitude) is present for the canonical density
used by NL93, $n_{\rm H}=10^{9.4}$~cm$^{-3}$. This jump is not seen at all
for much denser clouds.

Note, that the dust influence on the emission jump is much stronger in case
of Mg~II line than for H${\beta}$ line.
This difference is due to
the fact that the H${\beta}$ line forms in deeper parts of a cloud than Mg~II line.
In the presence of dust, the radiation reaching these depths is
harder since the dust opacity selectively removes lower energy photons,
allowing harder photons to reach the
region where H${\beta}$ is formed.
As a result, the H${\beta}$ forming region is warmer and
more ionized making the line stronger. Moreover, the
dust opacity is smaller at the wavelength
of H${\beta}$ than Mg~II, so H${\beta}$ is absorbed
less than Mg~II. This implies that the contribution of the NLR to the
overall line shape is expected to be lower in Mg~II than in H${\beta}$.

The He~II line emission vs radius from our simulations shows the luminosity jump
is at least one order of magnitude lower that the jump reported by NL93 for the same line.
Our simulations show that this jump is much smaller, only a factor of two, for three Sy1 SEDs,
and completely disappears in the case of the NLSy1 continuum.
Those differences may be caused by the different numerical code used by those authors.
Nevertheless, with the high density case, He~II line suppression is not
present for all considered  shapes of radiation.

For both densities, the C~III] line strongly depends on the SED shape.
With the   NLSy1 PMN J0948+0022 SED and the dust presence, line luminosity slowly decreases
with distance by $\sim$few factors, and the maximum line emission always occurs at $r<0.1$~pc.
In case of the Sy1 SEDs, the line luminosity peaks at $r \sim 10$~pc, with clear suppression at the
sublimation radius for the low-density case.

The  [O~III] emission (blue crosses in Figs.~\ref{fig:line_profile},
and \ref{fig:line_profile_hd}) reaches a maximum  farther outside the
sublimation radius. For the high density case,
this line is very weak in comparison with other lines. This is in agreement with
the fact that forbidden lines originate from low density gas.
Only for low density case there is  enhanced
[O~III] emission in a region close to the NLR ($r~\sim$10~--~100 pc). We expect that such line
will never be observed in the ILR. Indeed, the initial claim of the [O~III] variability
was not supported by the careful analysis of the data \citep{barth2016}.
Beside forbidden [O~III] line, our results strongly support the presence of an ILR
 where the intermediate velocity lines are expected.

\subsection{Apparent gap suppression}

To investigate  the role of  density in the formation of the ILR, we calculated
our model for several values of density normalizations:
$n_{\rm H}=10^{7.0},~ 10^{9.4},~ 10^{10.0}, ~ 10^{11.0},~ 10^{11.5}$~cm$^{-3}$,
keeping other parameters the same.
Fig.~\ref{fig:varden} shows the dependence of
line luminosity radial profiles on the density normalization for two representative
SEDs: Mrk 509 (left panels)
and PMN J0948+0022 (right panels), for all lines considered by us.

For the rare clouds, the luminosity of some lines decreases many orders of magnitude.
Those lines would
not be observed due to the sensitivity of the telescopes.
Therefore, we mark the lower limit on the line luminosity above which line could be visible,
by the horizontal dashed line on each panel. We estimated this limit by assuming a Gaussian
 spectral profile  of the emission lines
on top of underlying continuum given by our SEDs. For
this calculation, spectral line width is set to the value corresponding
to Keplerian velocity at 1 pc ($\sim$ ILR radii), for a
BH mass $\sim 10^{8} M_{\odot}$.
It is rather hard lower limit on the observable
line luminosities since the simulated isotropic luminosities should be at least 10 times
higher (assuming 100\% covering factor).
Nevertheless, simulated line luminosities presented in Fig.~\ref{fig:varden} fall below this
limit in some cases, and those lines have no chance to be
detected.

Note, that for a given SED, there is a preferred value of density for which the line
emission is the greatest. For example; the H${\beta}$ luminosity increases with the density
normalization and is a maximum for $n{\rm_{H}=10^{11.5}~cm^{-3}}$  at distances
0.1 pc $< r < 0.4$ pc. The He II luminosity  peaks at $r < 0.1$ pc, and the maximum
emission occurs for the lower density, whose value depends on the SED shape.
In case of PMN J0948+0022 the luminosity peak
is lower by an order of magnitude than for Mrk 509
SED, and occurs for density $n_{\rm {H}}{\rm ~=~10^{7} ~cm^{-3}}$. This is in
agreement with Locally Optimised Cloud (LOC) model
of \citet{baldwin1995}.

The radial distances at which the H${\beta}$ and He~II emissions are the strongest are
in agreement with the results inferred from the reverberation studies of the BLR in AGN.
The radial stratification with ionization potential of the species producing the line has been
observed \citep[i.e.][]{clavel1991,peterson1999}, showing
that He~II line always originates at distances closer by a
factor of three/four to the nucleus than H line.
In addition, the distances for which the luminosities of Mg~II
and [O~III] peaks are consistent with the reverberation
mapping studies.

For the Mrk 509 SED, the emission, with density normalization
$n_{\rm {H}}{\rm ~=~10^{7} ~cm^{-3}}$ at 0.1 pc, is insignificant for
all considered lines. However, the [O~III] emission is the
strongest for the PMN J0948+0022 SED with the lowest
density , which agrees with the prediction that forbidden
lines are formed in low density gas. For both SEDs, the
semi-forbidden line C~III] has a maximum emission at
intermediate densities i.e, $n_{\rm {H}}{\rm ~=~10^{9.4} ~cm^{-3}}$ at 0.1 pc.

Despite of the different distances where the line luminosities peak the strong jump
in the emission profiles disappears in almost all cases for both shapes of continuum,
when density normalization increases. The lack of this jump clearly means that there will
not be a gap between the BLR and NLR. This naturally explains the
origin of the intermediate line region.

\subsection{The connection with an accretion disk}

\begin{figure}
\hspace{-0.4cm}
\includegraphics[width=0.54\textwidth]{density_mass_accrate_paper.eps}
\caption{\small The accretion disk atmosphere density radial profiles.
The vertical dashed line marks the position of the sublimation radius. Straight lines are
plotted according to the power-law given in Eq.~\ref{eq:params} by the first term for
two different density normalization marked at the figure. Two datasets are
presented for expected masses and
Eddington ratios derived from an assumed bolometric
luminosity ($10^{45}$ erg~s$^{-1}$, see text for details).}
\label{fig:disk}
\end{figure}

It is widely believed that broad line emission clouds may be connected
with the wind from an accretion disk atmosphere
\citep{gaskell2009,czerny2011}.
The upper atmospheric layers of the disk can be quite dense, with value up to
$n_{\rm H} \sim 10^{14}$~cm$^{-3}$, depending on the distance from the central black hole
\citep{hrynio2011,rozanska2014}.  These densities are derived
by solving for the accretion disk vertical structure in hydrostatic and radiative equilibrium
parametrized by the black hole
mass, its spin, and the accretion rate \citep{rozanska99}.
We can properly derive the density at the disk photosphere, i.e. at the optical
depth  $\tau \sim 2/3$, assuming energy generation via viscosity, and diffusion
approximation of the radiative transfer.
Our calculations use the  Rosseland mean opacity tables from
\citet{alexander83,seaton94}. Those opacities are crucial for calculating the disk
density  since the true absorption opacity can be an order of magnitude
higher than electron scattering opacity as shown by
\citet[][see their Fig.~4 and 7]{rozanska99}.

We take the density at $\tau=2/3 $ as a representative of the initial
density in the disk wind, which supplies matter to the BLR or intrinsic absorbers in an outflow.
The model fully takes into account the radial
 transition from pressure dominated regions to gas dominated regions by assuming that the
viscous torque is proportional to the total pressure (gas and radiation), and we use realistic
description of the opacities, including atomic transitions and the presence of the dust. Nevertheless,
the model should not be extended too far beyond a $\sim 1$ pc scale because there the self-gravity
effects as well as the effects of the circumnuclear stellar cluster become important
\citep{thompson2005}.

The disk atmosphere radial density profile at $\tau=2/3$ is plotted in Fig.~\ref{fig:disk}.
We used two test sets of parameters. Keeping the bolometric luminosity constant
at $10^{45}$~erg~s$^{-1}$ we find the Eddington ratio for
masses of $10^7 M_{\odot}$ and $10^8 M_{\odot}$.
We can assume that our rescaled  SEDs should be produced in AGNs with BH masses in this range.
For the given assumptions and taking a radiative efficiency of 0.1 we then derive the Eddington
ratios corresponding to those masses: 0.8  and 0.08 respectively. In addition, the density of
the clouds used in our BLR-NLR simulations is drawn by straight lines according to
Eq.~\ref{eq:params}, for two normalizations at the sublimation radius:
$n_{\rm H} = 10^{9.4}$, and $10^{11.5}$ cm$^{-3}$.

It is thus clearly seen, that accretion disk atmospheres
naturally produce high densities at the sublimation radius. All models show a strong change in
density produced by heavy element Rosseland mean opacities used in our calculations.
Even if this bump
is slightly inside sublimation radius assumed by us, the
density radial profiles show that high densities occur in
the disk atmosphere, and such dense gas can give rise to the line emitting regions.

On the other hand, the local density at the disk atmosphere does not depend
on the Eddington ratio, and is expected to be the same
for the Sy1 and NLSy1 galaxies. Thus the differentiation in the local density
between those two types of objects must happen at the wind formation stage.
Smooth wind outflow causes the decrease of the density with the distance measured
along the wind stream line due to wind acceleration and the geometrical divergence
of the wind line. However, if thermal instability operates in the wind and colder/denser
cloud forms the evolution of the wind density becomes very complex and dependent on the
heating and cooling efficiency. The difference between the wind developing in Sy1 and NLSy1
may be due to the difference in the basic wind velocity. A given disk radius, measured in cm
or pc, corresponds to larger value of the $r/R_{\rm Schw}$ in NLSy1 than in Sy1, the corresponding
Keplerian velocity is lower, and the wind velocity, which usually is of the same order, is also
smaller, leaving perhaps more time for the development of the thermal instability in the wind.
This would explain higher density of the clouds in NLSy1 than in Sy1. However, detailed
analysis of the time-dependent wind model is certainly beyond the scope of the current paper.

\section{Conclusions}
\label{sec:con}
Following the work of NL93, we performed
numerical simulations of photoionised gas in
AGN  emission line regions and derived the
line luminosity radial profiles for various major lines:
H${\beta}$ ${\lambda}$4861.36 \AA, He~II ${\lambda}$1640.00 \AA,
Mg~II ${\lambda}$2798.0 \AA, C~III] ${\lambda}$1909.00 \AA
~and [O~III] ${\lambda}$5006.84 \AA ~originating at different
distances from the central engine of the AGN.

On the basis of the line emission vs radius derived for four different
SED shapes of incident radiation, and for different density normalizations at the sublimation
 radius, we find the following:
\begin{enumerate}
\item The presence or absence of the Intermediate Line Region is not determined by the spectral
shape of the incident continuum. Different SEDs do produce considerably different
behaviour of the emission line radial profiles, due to the different amount of
extreme UV and soft X-ray photons in its broad band SED. However these differences
do not adequately explain why an intermediate line emission is observed in some objects.
\item With higher densities normalization, i.e., n$_{H}$=10$^{11.5}~\rm{cm^{-3}}$ at $r=0.1$~pc,
we obtained flat luminosity line radial profiles for almost all lines and SEDs.
Thus, the dust does not suppress the line emission, contrary to the result obtained
by NL93. Our model potentially explains the existence of ILR in some sources. If the density
of the gas is high enough, emission lines of intermediate velocity width can be produced.
\item Such ILR is predicted to be located at radial distances $r \sim 0.1-1$ pc, and
the expected by our model the reverberation mapping lag would be of the order of 100-1000 light-days.
\item We demonstrated the dependence of line luminosity profiles on the density normalization.
We found that the significant line emission in objects with a particular SED occurs at different
densities in agreement with reverberation mapping studies of H${\beta}$, Mg~II, [O~III] and He~II
lines.
\item  We showed that dense clouds postulated by us can be potentially formed from an accretion disk
atmosphere which is dense enough below the sublimation radius in the accretion disk. This work is
another proof that the high densities occur in the BLR, which is in full agreement with many previous studies.
\end{enumerate}

\acknowledgments
{\small
We are grateful to Jonathan Stern, the referee, for very helpful
comments to the manuscript, and we thank Ari Laor and Jian-Min Wang
for helpful discussion. This research was supported by Polish National Science
Center grants No. 2011/03/B/ST9/03281, 2015/17/B/ST9/03422, and
by Ministry of Science and Higher Education grant W30/7.PR/2013.
It received funding from the European Union Seventh Framework Program
(FP7/2007-2013) under the grant agreement No.312789.
T.P.A. received funding from NCAC PAS grant for
PhD students. BC acknowledges the grant
from Foundation for Polish Science through the Master/Mistrz program 3/2012.
GJF thanks the Nicolaus Copernicus Astronomical Center for its hospitality
and acknowledges support by NSF (1108928, 1109061, and 1412155),
NASA (10-ATP10-0053, 10-ADAP10-0073, NNX12AH73G, and ATP13-0153),
and STScI (HST-AR- 13245, GO-12560, HST-GO-12309, GO-13310.002-A,
HST-AR-13914, and HST-AR-14286.001).
}

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


text:
Home Big Data MetaBeat: Activating in the metaverse when every dollar counts
MetaBeat: Activating in the metaverse when every dollar counts
Ed. note 10/4/22: Corrected Speedway sales figure from 200 million to 2 million in the sentence saying, "7-Eleven subsidiary Speedway is the most successful case study in the metaverse 'you've never heard of,' with 2 million in measurable sales from Atlas Earth to Speedway..."
MetaBeat, the metaverse event for enterprise decision-makers, started its day with a keynote introduction by Sami Khan, CEO and cofounder of Atlas Earth, a mobile game experience where users can purchase virtual real estate and brand partners can offer promotions tied to the company's in-app currency.
Right off the bat, Khan told the MetaBeat audience that no one can fully explain what the metaverse is, in all its iterations.
"My humble advice is to use the metaverse to enhance people's experience in the real world," he said. "I don't want my daughter growing up in a world where the future is escaping this world to live in a virtual reality world — that sounds pretty depressing."
Creating an enhanced experience in the real world, he explained, is different for every company. Nvidia, for example, is using digital twins as a metaverse to help teach future self-driving cars in a 3D world.
An enhanced real-world experience is the goal of Atlas Earth, he added, that is, using people's mobile devices to buy virtual land right where they live, work and play.
"We're taking local marketing to a national scale," he said. "It offers the ability for innovative brands like Sonic to drive a quarter-million in revenue from metaverse gamers to their doors." 7-Eleven subsidiary Speedway is the most successful case study in the metaverse "you've never heard of," with 2 million in measurable sales from Atlas Earth to Speedway, he added: "When you do this authentically people are excited about it."
After Khan's welcoming remarks, he brought up Ethan Chuang, VP of loyalty solutions at Mastercard Advisors and Mike Paley, EVP of business development at Atlas Earth, up for a Fireside Chat about activating the metaverse at a time when every dollar counts.
Paley, who was previously at popular browser extension Honey, which was acquired by PayPal for $4 billion, said that in his previous role he learned how important it is to deliver incremental value to your customers. "Even leveraging a simple piece of technology, I learned how incredibly transformative that could be to your user community," he said.
Mastercard, which links Atlas Earth to its loyalty program, is all about helping its business customers – merchants, CPGs, financial institutions — grow their businesses, Chuang said.
"What marketers and retailers are looking for is access to consumers in the channels of their choosing," he explained. "Consumers are moving away from traditional media — what you're doing in the metaverse, from the standpoint of extending reach to segments of the audience that a lot of retailers and marketers prize, is authentic dialogue. At the end of the day, the goal is to bring people into stores, into ecommerce and drive sales with a virtual circle."
Khan emphasized that he does not want the metaverse to be a "flash in the pan." That means building an ecosystem that builds positive value, he said.
"My hope is that everyone walks away today thinking about how marketers think about the metaverse," he said. "This ecosystem will continue to thrive when the economy flows through it. Understanding how they spend money is so important."
When every dollar counts, he asked the panelists, where does the thought process come in when it comes to spending money in an "experimental" channel like the metaverse?
Paley answered by saying he doesn't like the word "experimental channel." Instead, he said that Atlas Earth's efforts in the metaverse are not experimental, but build on previous performance marketing strategies.
"The program is set up so that brands are positioned for success from day one, especially as Mastercard gives us on their platform."
Mastercard's card linking strategy with Alpha Earth is an example of providing a frictionless experiment that makes it simple for users to take advantage of offers.
"You don't need to show anything at the point of sale, you're not constrained to digital or in store," he said, which is important in an era where gamers, and consumers generally, expect an instantaneous feedback loop.
Paley added that we live in a society based on instant gratification.
"In our experience, the metaverse is about bringing disparate parties together for real-time experiences – and anytime there is the opportunity to increase the value of the experience of the person having it in the real world, you're delivering on something special."
Still, a healthy metaverse — like any financially healthy ecosystem — requires the right balance.
"You need to find a home for marketing to make money to pay the other hand," he explained. "In the middle, I need a virtual cycle and an ecosystem that keeps growing."
The notion of metaverse is about to be tested, he cautioned.
"If markets keep going down, free money will dry up and our job is to challenge ourselves to think about how to build a healthy ecosystem as quickly as possible so we can count to move forward as the technology evolves," Paley said.
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As a travel photographer, once in a while I am treated to a sunset that is beyond spectacular. This one seemingly went on for hours and amazed all of us at the Terranea Resort as we lined up on the coastal bluffs to shoot creation's majesty.
This is yet another reason why we are madly in love with the SoCal coast.
Wish I could send you my sunset pictures. So close they could be the same picture!
If you have them posted anywhere on the Internet, you can put a link in here, and we'd be to see 'em.
Otherwise, thanks for stopping by and sharing your love of sunsets and Terranea.