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Tag: C.S.I (Page 1 of 2)
Greetings to the New Season: CBS – UPDATED
May 19, 2010 / Will Harris
Finally, things are starting to get interesting. CBS has released its schedule for Fall 2010, and, wow, talk about shaking things up. Thursday nights were already wreaking havoc on my viewing schedule, and now it's only going to get worse. Check out what the network has done, see what they've added to their line-up (including behind-the-scenes videos), and be sure to leave your comments below!
8 – 8:30 PM: How I Met Your Mother
8:30 – 9 PM: Rules of Engagement
9 – 9:30 PM: Two and a Half Men
9:30 – 10 PM: Mike & Molly: a comedy from Chuck Lorre ("Two and a Half Men," and "The Big Bang Theory") about a working class Chicago couple who find love at an Overeaters Anonymous meeting. Officer Mike Biggs (Billy Gardell) is a good-hearted cop who sincerely wants to lose weight. Mike's partner, Officer Carl McMillan (Reno Wilson), is a thin, fast-talking wise-guy, who despite his teasing encourages Mike on his road to slimness and romance. While speaking at an O.A. meeting, Mike meets Molly Flynn (Melissa McCarthy), an instantly likeable fourth-grade teacher with a healthy sense of humor about her curves.
For Molly, focusing on smart choices isn't easy because she lives with her sexy older sister, Victoria (Katy Mixon), and their mother, Joyce (Swoosie Kurtz), both of whom flaunt their healthy appetites and slender figures. Mike also faces temptation at the diner he and Carl frequent, where they've become friends with the Senegalese waiter, Samuel (Nyambi Nyambi), who finds trying to eat less a foreign concept. For Mike and Molly, thanks to their mutual love of pie and the desire to resist it, finding each other may have been worth the "weight." Chuck Lorre and Mark Roberts are executive producers.
10 – 11 PM: Hawaii Five-0: a contemporary take on the classic series about a new elite federalized task force whose mission is to wipe out the crime that washes up on the Islands' sun-drenched beaches. Detective Steve McGarrett (Alex O'Loughlin), a decorated Naval officer turned cop, returns to Oahu to investigate his father's murder and stays after Hawaii's governor persuades him to head up the new team: his rules, her backing, no red tape and full blanket immunity to hunt down the biggest "game" in town.
Joining McGarrett is Detective Danny "Danno" Williams (Scott Caan), a newly relocated ex-New Jersey cop who prefers skyscrapers to the coastline but is committed to keeping the Islands safe for his 8-year-old daughter; and Chin Ho Kelly (Daniel Dae Kim), an ex-Honolulu Police Detective wrongly accused of corruption and relegated to a federal security patrol, who is also a former protégé of McGarrett's father. Chin's cousin, Kono (Grace Park), is a beautiful and fearless native, fresh out of the academy and eager to establish herself among the department's elite. McGarrett vows to bring closure to his father's case while the state's brash new FIVE-0 unit, who may spar and jest among themselves, is determined to eliminate the seedy elements from the 50th state. Peter Lenkov, Alex Kurtzman and Roberto Orci are executive producers.
2010 Fall TV Preview, External Entertainment, External TV, Fall TV Preview, News, Pilots, Reality TV, TV, TV Action, TV Comedies, TV Dramas, TV Reality
$#*! My Dad Says48 Hours Mystery60 MinutesBlue BloodsC.S.ICrimetime SaturdayCriminal MindsCriminal Minds spinoffCSI MiamiCSI NYCSI: Crime Scene InvestigationHawaii Five-0HeadlinesHow I Met Your MotherMediumMike & MollyNCISNCIS: Los AngelesRules of EngagementShit My Dad SaysSurvivorThe Amazing RaceThe Big Bang TheoryThe DefendersThe Good WifeThe MentalistTwo and a Half MenUndercover Bossuntitled Criminal Minds spinoff
TV in the 2000s: The Shows that Defined the Decade
December 6, 2009 / Ross Ruediger
A recent issue of Time magazine has the phrase "The Decade from Hell" emblazoned across its front cover. It's referring to everything America has gone through in the past ten years, and it's difficult to argue such an assertion: it's been a shitty decade on a national level. During such times of stress, people inevitably turn to entertainment as a form of release, and although the methods in which we've distracted ourselves over the last ten years have unquestionably diversified, television remains the most easily accessible outlet for most Americans.
Within the format itself, the whole concept of reality TV must surely have been the biggest revolution of the decade. It's really easy to bag on reality TV – mostly because the bulk of it is so damned unreal – but anybody who spends any time in front of the tube has surely had at least a couple of reality series they consider appointment TV. The two concepts that paved the way for everything else are undoubtedly "Survivor" and "American Idol." The former, of course, opened the floodgates for the genre, and while it's seen a considerable dip in the ratings department over the years, 12 million viewers isn't a viewing figure to sneeze at. The latter, despite all the bitching and moaning and cries of "it's not as good as it used to be" that accompany each new season, remains one of the most watched shows on the tube, likely due to the fact that it's strictly a talent competition.
On "American Idol," the only backstabbers are the judges, and since they aren't part of the competition, their amusing duplicity is championed. The contestants, on the other hand, are innocents, and once the competition is underway, we're given no peek into any possible backstage drama, which is a good thing, because by the time the audition rounds are over, we've had enough drama to last the whole season. Everything that comes after is all about who can best transfix us for three minutes a week via one pop ditty. It actually says something positive about the U.S. that "American Idol" remains our #1 form of reality entertainment, even if the actual reality is that the vast majority of Americans couldn't care less about buying the winner's album six months after they're crowned.
You might think reality TV is a bunch of crap, and in most cases you'd be right, but the whole idea of it, to my mind, led to an important revolution, and that is serialized nighttime television (the classic "soap" formula notwithstanding). Reality shows taught viewers how to become invested in characters, how to be concerned for their eventual fate, and, most importantly, how to pay attention to an ongoing storyline, and the need to tune in every week. It didn't take long for the networks to figure out that there was an audience for shows that didn't continually hit the reset button. "24" must have been the first successful show of the decade to embrace the serial formula, and it embraced it whole hog. It required you to tune in for every episode, because each installment was another hour of a single day in the life of Kiefer Sutherland's Jack Bauer. That "24" premiered less than two months after the terrorist attacks on 9/11 was pure happenstance. That it became enormously popular with viewers? Probably not so much. America needed some fictitious reassurance that there were folks on the job who could get shit done, and "24" filled the prescription.
Strangely, "24" didn't open the network floodgates for more such programming right away. It took a few years, and then "Lost" made its mark. The number of "Lost" episodes I've seen could be counted on two hands, but that's not because I didn't like it, but because real life got in the way of it being appointment TV. Yet I viewed the pilot for "Lost" several months before its 2004 premiere, and when it ended I was convinced that I'd seen the second best TV pilot ever made. ("Twin Peaks" stills sits at #1.) The fact that a show as intricate as "Lost" still has a hardcore, central audience is perhaps a testament to that pilot. "24" started a new story with each new season; "Lost" required that you tune in for every episode of every season.
Another sci-fi series that did just that was "Battlestar Galactica," a show that, due it being on a niche network (Syfy), never amassed a huge audience yet snagged boatloads of publicity and awareness nonetheless. It was no small feat to take an utterly laughable short-lived series from the late '70s and re-envision it for modern audiences, but Ron Moore and company did just that…and they did it far more successfully that anyone ever guessed possible. Most amazingly, the show taught us a lot about ourselves, by thoroughly defining what it means to be human, and as the damaged '00s dragged on, there may not have been a more important lesson to be learned.
On the same day I saw the "Lost" pilot, I saw another pilot for a completely different kind of series. While I didn't rank it as one of the greats, there was one thing I was sure of: it would be a massive hit…and it was. "Desperate Housewives" was precisely the sort of vapid, soapy fare that had been absent for far too long on American TV. It clued into the seemingly bland suburban construct which surrounds so many Americans, via the Lynchian notion that "all is not what it seems." Most anyone who lives a suburban life can no doubt relate to that idea, because wherever there are groups of people, there are bound to be some of them that are fucked up. "Housewives" is littered with fucked up suburbanites of all shapes, sizes and types, but they're kooky and funny and there's always some twinkly music playing in the background that in the end makes everything OK. It is not great television, but over the years it has, for the most part, been immensely watchable in the most disposable sort of way.
Around the same time period as "Housewives," "Grey's Anatomy," made some major waves. It's a series I have never watched and never plan to, but I'd be foolish to omit it from discussion since it brought two annoyingly obnoxious terms to the TV table: McDreamy and McSteamy. I haven't heard either in a few years, but there was a time when they seemed to define everything that was wrong with television. I assume "Grey's" fans have grown out of it…or maybe the show killed one of those guys off? I've no idea and can't be motivated to investigate. Presently, there's a brand new version of it going around, through cinema, via Camp Edward and Camp Nimrod. People can be so easily distracted it makes you wonder why some shows actually try harder.
24, American Idol, Battlestar Galactica, Curb Your Enthusiasm, Desperate Housewives, External Entertainment, External TV, Lost, Mad Men, South Park, The Office, The Shield, The Sopranos, The Wire, TV, TV Action, TV Comedies, TV Dramas, TV Reality, TV Sci-Fi
24American IdolArrested DevelopmentBattlestar GalacticaBoston LegalC.S.ICurb Your EnthusiasmDesperate HousewivesEnd of Decade TVFamily GuyGrey's AnatomyHouseLostMad MenMonkNip/TuckSex and the CitySix Feet UnderSouth ParkSurvivorThe Colbert ReportThe Daily Show with Jon StewartThe OfficeThe ShieldThe SopranosThe Wire
Box office can be bad all by itself (updated)
And by "bad" I might actually mean "good" for at least one, perhaps two, of the four new major releases coming this first weekend of the traditional movie fall season.
First off, jolly Carl DiOrio of THR is bullish as he anticipates about $20 million for the latest from Tyler Perry, the hyphenate auteur whose major appeal to African-American audiences, and major lack of appeal to critics, has been proven several times. His latest film version of one of his hit plays, "I Can Do Bad All By Myself," is not being screened for the nasty folks of the press. The latest appearance of Madea, Perry's chunky female alter-ego, is nevertheless thought to be attracting interest with his usual blend of melodrama, broad comedy, and music. (Having both Mary J. Blige and the great Gladys Knight in the cast won't hurt this one.)
For cinephiliacs and geeks, the most interesting release this week by far is the computer animated dystopian science-fiction fable, "9" — which is not to be confused with the upcoming musical stage adaptation, "Nine." This may seem a bit odd, but it gets downright weird. I just did little searching on IMDb and found two other films named "9" (not counting director Shane Acker's original short subject). I also found a total of six films entitled "Nine," including the upcoming musical version of Felini' s "8 1/2" starring Danel Day Lewis and Marion Cotillard and directed by Rob Marshall. That makes six films named "Nine" and three films named "9" which, of course, comes to nine films called "9" or "Nine." That either means the apocalypse is nigh this November 25 when the musical "Nine" comes out or, the moment of its release, I should go to Vegas, head straight for the crap tables, and bet everything on hitting 9. How can I lose?
As for Shane Acker's, "9," though it's been the beneficiary of some buzz, I personally wouldn't bet everything on the dark tale finding a huge foothold with audiences. With a PG-13 rating, a vision clearly too scary for small children, and characters who a friend of mine — who really wanted to see it — likened to a jock strap, this film would be risky even if it was tremendous. However, David Medsker's mixed review seems pretty much in line with the unspectacular 60% "Fresh" Rotten Tomatoes rating; the consensus being that this expansion of a short film is weak on story though strong on compelling visuals. "9" actually opened Wednesday and made about $3 million. Expectations are fairly high, with DiOrio suggesting the film could reach $15 million, even though the theater count is a relatively modest 1650+.
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9All About SteveC.S.IGladys KnightI Can Do Bad All By MyselfI Know What You Did Last SummerKate BeckinsaleMary J. BligeNightwatchNineRev. Marvin WinansSandra BullockSorority RowThe ThingTyler PerryVery Bad ThingsWantedWhiteout
TCA Tour: CBS Executive Session
Nina Tassler, President of CBS Entertainment, has honored us with her presence this morning at CBS's TCA day, and during her executive session, she provided us with the following tidbits:
* When word leaked out – that's hardly the right phrase, since it was actually included in a network-provided schedule, but we'll go with it, anyway – that there would be a "Mystery Panel" today, hopeful (perhaps overly optimistic) critics began theorizing that it would be for "The Late Show with David Letterman." As it turns out, it's actually for CBS's upcoming revival of "Let's Make A Deal," which Nina briefly detailed for us. It'll be hosted by Wayne Brady and will premiere on October 5th. And, yes, Monty Hall is involved, but only as an executive producer. Come on, though: an old pro like that surely won't be able to resist rearing his head onscreen once in awhile. I think we can count on him to show up during Sweeps Week, at the very least.
* Of NBC's great Jay Leno experiment, she says, "Whatever ratings they get, they're going to declare victory, so it really doesn't matter." As far as CBS goes, however, they're going to stick with the successes of their 10 PM dramas. (Good plan.) She also got a laugh when she admitted that she thought that NBC's announcement that Conan O'Brien was the new king of late night "seemed premature."
* Rocky Carroll will be a recurring character on the new "NCIS: Los Angeles," but Pauley Perrette will be guesting in the show's second episode.
* There are nine more "Flashpoint" episodes yet to be aired, and they're still happy with the way the arrangement of airing a Canadian-produced series on American TV. As such, "The Bridge" will be turning up on CBS in the near future as well. But there are no plans yet to produce any further "Flashpoint" episode, although she says they reserve the right to do so.
* As far as "Harper's Island" goes, it had some online traction and appealed to a niche audience. "The challenge is to find something that can appeal to niche but that has a broader appeal as well," she said. She was happy with the series, but "it just didn't grab on to a bigger audience."
* Apparently, "CSI" fans' biggest issue with Laurence Fishburne was that he needed to look "more comfortable in his clothes." You will be pleased to learn that this is being taken care of.
* No plans for any more "Million Dollar Password" at the moment.
* Her one-liner about Ben Silverman's departure from NBC: ""I'm really just a D girl, so I wouldn't comment."
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Ben SilvermanC.S.ICBSConan O'BrienFlashpointHarper's IslandJay LenoLaurence FishburneLet's Make A DealMillion Dollar PasswordMonty HallNCISNCIS: Los AngelesNina TasslerPauley PerretteRocky CarrollTCA Blog 2009TCA Press TourThe BridgeWayne Brady
CBS: The Fall Schedule
Well, I know at least one person who is beside herself about the news that Alex O'Loughlin is back on the airwaves, but I'm obviously happiest to get the confirmation that CBS did indeed decide to pick up "Medium" after NBC so rudely dumped it, giving it the most appropriate timeslot on their schedule (the post-"Ghost Whisperer" spot on Friday nights). Let's look at the rest of the developments, shall we?
8:00 PM – How I Met Your Mother
8:30 PM – Accidentally On Purpose
A comedy starring Golden Globe Award winner Jenna Elfman as Billie, a single woman who finds herself "accidentally" pregnant after a one-night stand with a much younger guy, and decides to keep the baby… and the guy. A newspaper film critic, Billie is barely surviving a humiliating breakup with her charming boss, James (Grant Show), who's still trying to resume their relationship. Suddenly expecting a child with her "boy toy," Zack (Jon Foster), Billie and Zack make an arrangement: to live together platonically. Billie's party girl best friend Olivia (Ashley Jensen), and Abby (Lennon Parham), her conventional, younger married sister, eagerly look forward to the new addition and offer their own brands of advice and encouragement. But when Zack and his freeloading friends, including Davis (Nicolas Wright), start to turn her place into a frat house, Billie isn't sure if she's living with a boyfriend, a roommate, or if she just has another child to raise.
9:00 PM – Two and a Half Men
9:30 PM – The Big Bang Theory
10:00 PM – CSI Miami
8:00 PM – NCIS
9:00 PM – NCIS: Los Angeles
A drama about the high stakes world of undercover surveillance at the Office of Special Projects (OSP), a division of NCIS that is charged with apprehending dangerous and elusive criminals that pose a threat to the nation's security. By assuming false identities and utilizing the most advanced technology, this team of highly trained agents goes deep undercover, putting their lives on the line in the field to bring down their targets. Special Agent "G" Callen (Chris O'Donnell) is a chameleon who transforms himself into whomever he needs to be to infiltrate the criminal underworld. His partner is Special Agent Sam Hanna (LL Cool J), a former U.S. Navy SEAL who has seen action in both Afghanistan and Iraq, and a surveillance expert who uses state of the art monitoring equipment to look out for those in the field and feed them crucial information. Both Callen and Hanna report to Special Agent Lara Macy (Louise Lombard), the OSP team leader responsible for directing the operations and making life-or-death decisions. Assisting the team is Special Agent Kensi Lo (Daniela Ruah), the exceptionally bright daughter of a slain Marine who lives for the adrenalin rush that comes with undercover work, and Operational Psychologist Nate Getz (Peter Cambor), adept at getting into anybody's head, profiling the target and monitoring agents' states of mind before, during and after missions. Armed with the latest in high tech gear and sent regularly into life-threatening situations, this tight-knit team relies on each other to do what is necessary to protect national interests.
10:00 PM – The Good Wife
A drama starring Emmy Award winner Julianna Margulies as a wife and mother who must assume full responsibility for her family and re-enter the workforce after her husband's very public sex and political corruption scandal lands him in jail. Pushing aside the betrayal and crushing public humiliation caused by her husband Peter (Chris Noth), Alicia Florrick (Margulies) starts over by pursuing her original career as a defense attorney. As a junior associate at a prestigious Chicago law firm, she joins her longtime friend, former law school classmate and firm partner Will Gardner (Josh Charles), who is interested to see how Alicia will perform after 13 years out of the courtroom. Alicia is grateful the firm's top litigator, Diane Lockhart (Christine Baranski), offers to mentor her but discovers the offer has conditions and realizes she's going to need to succeed on her own merit. Alicia's main competition among the firm's 20-something new recruits is Cary (Matt Czuchry), a recent Harvard grad who is affable on the surface, but will use any means to ensure that he, not Alicia, secures the one full-time associate position that's available. Fortunately, Alicia finds an ally in Kalinda (Archie Panjabi), the firm's tough in-house investigator. Gaining confidence every day, Alicia transforms herself from embarrassed politician's scorned wife to resilient career woman, especially for the sake of providing a stable home for her children, 14-year-old Zach (Graham Phillips) and 13-year-old Grace (Makenzie Vega). For the first time in years, Alicia trades in her identity as the "good wife" and takes charge of her own destiny.
External Entertainment, External TV, Fall TV Preview, News, Reality TV, TV, TV Action, TV Comedies, TV Dramas, TV Reality
48 Hours Mystery60 MinutesAccidentally On PurposeAlex O'LoughlinArranged MarriageC.S.ICold CaseCrime Time SaturdayCriminal MindsCSI MiamiCSI NYCSI: Crime Scene InvestigationGary UnmarriedGhost WhispererHow I Met Your MotherMediumMiami TraumaNCISNCIS: Los AngelesNumb3rsRules of EngagementSurvivorThe Amazing RaceThe Big Bang TheoryThe BridgeThe Good WifeThe MentalistThe New Adventures of Old ChristineThree RiversTwo and a Half MenUndercover Boss


text:
\section{Introduction}
\pagestyle{myheadings}
\markboth{\small Ganguly et al. \hfill Intrinsic Quasar Absorbers~~}
         {\small Ganguly et al. \hfill Intrinsic Quasar Absorbers~~}

Absorption by an ionized medium close to the central engine is now
recognized as a fairly common feature in the spectra of active
galactic nuclei (hereafter AGNs). In Seyfert~1 galaxies, the signature
of the ionized gas takes the form of narrow UV resonance absorption
lines from highly--ionized species, such as {\hbox{{\rm N}\kern 0.1em{\sc v}}} and {\hbox{{\rm C}\kern 0.1em{\sc iv}}} (Crenshaw,
Maran, \& Mushotzky 1998\nocite{cmm98}) as well as soft X--ray
absorption edges from highly ionized species such as {\hbox{{\rm O}\kern 0.1em{\sc vii}}} and
{\hbox{{\rm O}\kern 0.1em{\sc viii}}} (\cite{reyn97}; \cite{geo98}).  Similar UV absorption
lines\footnote{Here, we consider only absorption lines which are close
to the redshift of the quasar, i.e.  {${z_{\rm abs}}\approx{z_{\rm em}}$}, not lines
at considerably lower redshifts than that of the quasar.} are also
observed in quasars (e.g. \cite{foltz86}; \cite{and87}; Young,
Sargent, \& Boksenberg 1982\nocite{ysb82}; Sargent, Boksenberg, \&
Steidel 1988\nocite{sbs88}; \cite{ss91}).  Quasars, however, are
perhaps better known for their {\it broad} absorption lines, whose
widths often reach {50,000~\hbox{km~s$^{-1}$}} (e.g., \cite{turn88};
\cite{wey91}). The high ionization state of the absorbers and the
often blueshifted absorption lines (relative to the broad emission
lines) suggest that the absorber is a fairly tenuous medium outflowing
from the AGN, most likely accelerated by radiation pressure
(\cite{arav95}). The absorber could plausibly be associated with an
accretion--disk wind (e.g.,
\cite{mur95}; \cite{kk95}) analogous to those observed
in many cataclysmic variables (e.g., \cite{drew90}; \cite{mauche94}).
This can only be a broad analogy, however, since a number of
observational clues suggest that the picture in AGNs is neither as
simple nor as ``clean'' as in cataclysmic variables. For example, the
fact that absorption line depths often exceed either the net continuum
level or the net emission--line level on which they are superposed
suggests that the absorber does not lie between the broad
emission--line region (BELR) and the more compact continuum source
since it intercepts both continuum and emission--line photons. That is,
it lies either within the BELR or away from both regions.

The relation between the absorption--line region and the ubiquitous AGN
emission--line regions is unknown, although it has been suggested that
they may represent different phases or layers of the same medium
(Shields, Ferland, \& Peterson 1995\nocite{shields95};
\cite{ham98}). From an observational perspective, it is important to
determine the geometry of the absorbing gas and its physical
conditions because these constitute useful constraints on theoretical
models of the ionization and acceleration of the outflow.  Moreover,
it is also interesting to ask whether there are any trends in the
properties of the absorption lines with AGN subclass since such trends
serve as constraints on scenarios of fundamental differences between
such subclasses (e.g., the radio--loud/radio--quiet AGN dichotomy).  It
is, therefore, encouraging that some progress has been made in recent
years in answering the above questions. First, observations of large
samples of quasars indicate that {\it broad} absorption lines (BALs)
are found preferentially among radio--quiet quasars (\cite{stocke92}),
while the preferred hosts of associated
\footnote{``Associated'' absorption lines, according to the definition of
Anderson {et~al.}~(1987\nocite{and87}), are
those with velocities within {5000~\hbox{km~s$^{-1}$}} of the quasar rest frame. In
principle, associated absorption lines need not be intrinsic to the
quasar.}
{\it narrow} absorption lines (NALs) are radio--loud quasars
(\cite{foltz86}; \cite{and87}).  These trends are by no means
well--established and have been called into question by the discovery
of radio--loud BAL quasars (\cite{beck97}; \cite{broth98}) and
radio--quiet intrinsic NAL quasars (Hamann, Barlow, \& Junkkarinen
1997a\nocite{ham97a}; \cite{ham97b}).
We note, however, that the Foltz {et~al.}~(1986\nocite{foltz86})
and Anderson {et~al.}~(1987) results discuss the preference of
{\it strong} associated NALs for radio--loud quasars, while also
demonstrating that weak associated NALs occur in both radio--quiet
and radio--loud quasars.
Second, observations of
selected NAL quasars at high spectral resolution have shown that the
absorbers only partially cover the background BELR and/or continuum
source (\cite{bs97}; \cite{ham97a}). In another quasar, the NALs were
found to vary on a time scale of only a few months
(\cite{ham97b}). These observations demonstrate that the NALs in these
objects are intrinsic and also provide useful constraints on their
geometry.

In this paper, we present five associated NALs along the lines of
sight toward six quasars observed at high spectral resolution. These
were discovered serendipitously in a survey of {\it intervening} {\hbox{{\rm Mg}\kern 0.1em{\sc ii}}}
absorbers ({${z_{\rm abs}} \ll {z_{\rm em}}$}; \cite{cwcthesis}). In three of the five
cases, the NAL systems exhibit the partial coverage signature of
absorbing gas {\it intrinsic} to the quasar. In the process of
analyzing the data, we have refined and expanded the method of Barlow
{\&} Sargent~(1997\nocite{bs97}) to treat the coverage fractions of
the continuum source and the BELR separately. Although it is, in
principle, impossible to determine the two coverage fractions
independently using an absorption doublet, it is possible to place
interesting constraints on them. In particular, we find that in two of
the quasars in this small collection, the continuum source must be
partially covered by the absorber.

In \S2 of this paper, we describe the selection of the original quasar
sample, the observations and data reduction, and the properties of the
associated NALs that we detected and other relevant properties of
their hosts. In \S3 and \S4, we show that, in three of these systems,
the relative strengths of the absorption lines provide evidence for
partial coverage of the background source by the absorber. In \S4, we
determine the effective coverage fractions by applying the method of
Barlow \& Sargent (1997\nocite{bs97}). We also develop and apply a
refined version of this method in which we treat the coverage fraction
of the continuum source and broad BELR separately. In \S5, we discuss
the implications of the observational results, possible partial
coverage mechanisms, and the general picture of intrinsic absorbers in
different types of active galaxies. In \S6, we summarize our findings
and present our final conclusions.

\section{Sample of Objects, Observations, and Data}

The associated NAL systems reported here were found in the course of a
large statistical study of intervening {\hbox{{\rm Mg}\kern 0.1em{\sc ii}}} absorbers during which
spectra of a sample of 25 quasars were obtained (\cite{cwcthesis}). In
six objects from this sample, the spectra included the broad {\hbox{{\rm C}\kern 0.1em{\sc iv}}}
emission line and revealed the presence of five associated NAL systems
within {$5000$~\hbox{km~s$^{-1}$}} of the emission--line redshift.  Another system at
$\Delta v = -13,800~{\hbox{km~s$^{-1}$}}$ toward Q~$0450-132$ could be
``associated'' (see Petitjean, Rauch, \& Carswell 1994\nocite{pet94}),
but it does not satisfy the traditional velocity criterion. These six
quasars are listed in Table~\ref{tab:qso} along with the some of their
basic properties. The emission redshifts and emission line fluxes for
the quasars were taken from Sargent {et~al.}~(1988\nocite{sbs88}) and
from Steidel \& Sargent (1991\nocite{ss91}). Because of the way the
original sample was selected, the final collection of six quasars
whose {\hbox{{\rm C}\kern 0.1em{\sc iv}}} emission lines were observed is unbiased towards the
presence of associated {\hbox{{\rm C}\kern 0.1em{\sc iv}}} NALs. In two of the six objects the
spectra include additional absorption lines, namely {\hbox{{\rm Si}\kern 0.1em{\sc iv}}} and {\hbox{{\rm N}\kern 0.1em{\sc v}}}
in Q~$0450-132$ and {\hbox{{\rm Si}\kern 0.1em{\sc iv}}} in Q~$1213-003$.

Since the radio properties of these quasars are important to our later
discussion, we have compiled information about their radio properties
based on reports in the literature and included it in
Table~\ref{tab:qso} along with the appropriate references. The observed
5~GHz radio flux was converted to the rest frame of the source using
the measured spectral index $\alpha$, if available, or assuming
$\alpha=0.5$ otherwise (where $f_{\nu}\propto \nu^{-\alpha}$). The
radio power was computed assuming a Hubble constant of 50~${\rm
km~s^{-1}~Mpc^{-1}}$, and a deceleration parameter of ${1\over 2}$,
following Kellermann {et~al.}~(1994\nocite{kel94}). The rest--frame
4400~{\AA} optical flux was calculated from the observed $V$ magnitude
assuming a flat optical--UV spectrum (i.e., $\alpha=0$;
\cite{elvis94}). To classify an object as radio--loud or radio--quiet, we
adopted the criteria of Kellermann {et~al.}~(1994\nocite{kel94})
according to which radio--loud quasars have either a 5~GHz power of
$P_{\rm\, 5~GHz} > 10^{26}~{\rm W~Hz}^{-1}$ or a 5~GHz--to--4400~{\AA}
flux density ratio of $R>10$.  According to these criteria, three of
the six objects are radio--quiet and three are radio loud.

The observations were carried out with the HIRES spectrometer
(\cite{vogt94}) on the Keck~I telescope. The spectra have a resolution
of 6.6~{\hbox{km~s$^{-1}$}} with a sampling rate of 3 pixels per resolution
element.  They were reduced with the IRAF\footnote{IRAF is distributed
by the National Optical Astronomy Observatories, which are operated by
AURA, Inc., under contract to the NSF.} {\tt apextract\/} package for
echelle data.  The detailed steps for the reduction are outlined in
Churchill (1997\nocite{cwcthesis}).

The details of the observations are listed in Table~\ref{tab:obs}
which also includes the parameters of the associated NAL systems that
we detected along with the lowest measurable equivalent widths
($5\sigma$ limits) in the corresponding spectrum. In this table, we give
the mean velocity of each absorption--line system relative to the peak
of the broad emission line.  NALs were found at both negative
(blueshifted) and positive (redshifted) velocities relative to the
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} broad emission--line peak. A positive velocity, such as seen in
{PG~$1222+228$} and {PG~$1329+412$}, need not imply infall toward the
quasar since the true velocity of the quasar is more accurately
measured by narrow forbidden lines than by the broad emission line
peaks. For example, in a picture in which the NAL gas is outflowing from the
central engine, the NAL redshift would imply a smaller outflow
velocity of the absorbers relative to the broad emission--line gas.

Figures \ref{fig:q0450f1}--\ref{fig:q1329f1} present the velocity
aligned absorption profiles of the {\hbox{{\rm C}\kern 0.1em{\sc iv}}} doublets and of other
detected transitions ({\hbox{{\rm Si}\kern 0.1em{\sc iv}}} and {\hbox{{\rm N}\kern 0.1em{\sc v}}}) of the five associated
systems that were covered in the HIRES/Keck~I spectra.  The
{\hbox{{\rm C}\kern 0.1em{\sc iv}}}$\lambda$1550 profile of the {$\Delta v=-60$~\hbox{km~s$^{-1}$}} system of
{Q~$1213-003$} (Figure~\ref{fig:q1213f2}) is truncated near 0~{\hbox{km~s$^{-1}$}}
because is falls off the edge of the CCD. In fact, because of the
redshift of {Q~$1213-003$} its {\hbox{{\rm C}\kern 0.1em{\sc iv}}} emission line is in the
observed wavelength range above 5100~\AA, where the echelle orders are
separated by gaps. As a result, there are several gaps in the coverage
of the broad emission--line profile. None of the other objects suffer
from this problem, however.

The kinematic structure of the NAL profiles is varied and has multiple
components. It is not distinguishable from the structure found in
intervening absorbers.  However, the strong {\hbox{{\rm N}\kern 0.1em{\sc v}}} absorption in
{Q~$0450-132$} is indicative of the typically high metallicities of
associated systems (\cite{pet94}) in contrast to the lower
metallicities of intervening systems.  In \S3 and \S4, we demonstrate
that in three of the five systems there is evidence that the absorbing
clouds only partially cover the source, which then requires them to be
in relatively close proximity to the source. It should be noted that
the {$\Delta v=-60$~\hbox{km~s$^{-1}$}} system of {Q~$1213-003$} has been classified
as intrinsic by Sowinski, Schmidt, \& Hines (1997\nocite{sow97}), but
we have not been able to find the relevant report in the literature.

\section{Identification of Anomalous Optical Depths}

In the three of the quasars displaying NALs we find that the optical
depth ratio of the two members of the {\hbox{{\rm C}\kern 0.1em{\sc iv}}} doublet did not have the
value expected from atomic physics, namely {${{\tau_1} \over {\tau_2}}
={{f_1 \lambda_1} \over {f_2 \lambda_2}}$} (\cite{sav91}; where $f_1$
and $f_2$ are the oscillator strengths and $\lambda_1$ and $\lambda_2$
are the rest wavelengths of the doublet members). To demonstrate this
discrepancy, we have fitted the weaker member of each doublet with a
combination of Voigt profiles, scaled the model according to what
atomic physics dictates for the stronger member of the same doublet,
and compared it to the data. The results of this exercise are
illustrated in Figures~\ref{fig:q0450f1}--\ref{fig:q1329f1}, where we
show the models as solid lines superposed on the data. The bottom
panel in each set shows the deviation of the data from the predicted
profile of the strongest member of each doublet in each resolution
element, scaled by the error bar.  We see three obviously discrepant
cases: the $\Delta v=-2011$~{\hbox{km~s$^{-1}$}} system toward Q~$0450-132$
(Figure~\ref{fig:q0450f1}), the $\Delta v=+1482$~{\hbox{km~s$^{-1}$}} system toward
PG~$1222+228$ (Figure~\ref{fig:q1222f1}), and the $\Delta
v=+314$~{\hbox{km~s$^{-1}$}} system toward PG~$1329+412$ (Figure~\ref{fig:q1329f1}).
Neither of the associated systems toward Q~$1213-003$ appear to
deviate from the atomic physics prediction.

We consider five explanations for the apparent violation of the
optical depth scalings in these three associated systems: (1) an
instrumental/reduction effect such as scattered light which mimics a
source function (e.g., \cite{cmm98}) (2) blends with other transitions
at other redshifts; (3) a source function that fills in the line cores
(Wampler, Chugai, \& Petitjean 1995\nocite{wam0059}); (4) incomplete
occultation of the continuum and/or emission--line by the absorbers
(Wampler, Bergeron, \& Petitjean 1993\nocite{wam2116};
\cite{wam0059}; Hamann {et~al.}~1997a,b\nocite{ham97a}\nocite{ham97b};
\cite{bs97}) and (5) scattering of background photons back into the light path.
The first
is an unlikely resolution to the problem since the optical depth
scaling is obeyed by all 64 intervening absorption--line systems
(including transitions from {\hbox{{\rm C}\kern 0.1em{\sc iv}}}, {\hbox{{\rm Mg}\kern 0.1em{\sc ii}}}, and {\hbox{{\rm Fe}\kern 0.1em{\sc ii}}}) observed
with the same instrumental setup and reduced in the same manner
(\cite{weakmgII}).  In addition, we have
searched the spectra of these quasars for an extensive set of
transitions at the redshifts of all other known systems, and found
that none of them affect the profiles studied here.  This rules out
the second possibility. Some forms of the source function explanation
could be viable while others are not; we consider these further in
\S5.2. The fourth and fifth explanations have identical signatures,
since we can think of scattering as a form of ``effective partial
coverage''.  Intuitively, the partial coverage effect will cause
models that assume full coverage to over--predict the strength of the
stronger member of a doublet, relative to the weaker.  Physically, the
intensity observed in the core of an absorption profile is the
composite of two types of light paths: (1) light that is not occulted
by the absorbing clouds or is scattered back into the light path, and
(2) the light that successfully passes through the absorbers.  The
unocculted fraction (in normalized units) is nearly the same for both
members of the doublet provided the emission line is not too steep
over the wavelength range covered by the absorption (see Appendix).
This results in a larger increase in the flux, relative to the full
coverage expectation, detected in the deeper blue member of the
doublet relative to the red member. The most straightforward example
is a situation in which the absorbers are optically thick such that
the unattenuated flux is negligible at either member of the doublet.
With partial coverage, one still observes a significant flux which is
equal in the two members.

\section{Partial Coverage}

\subsection{Effective Coverage Fraction $C_{\rm f}$}

To pursue the partial coverage interpretation further we have computed
the effective coverage fraction following Barlow \& Sargent (1997) and
Hamann {{et~al.}} (1997a). The effective coverage fraction is computed by
considering the fraction of all photons of a given wavelength that do
not pass through the absorbing gas. This calculation assumes a single,
{\it extended} continuum and emission--line source and a single
effective optical depth appropriate to the absorbing clouds at the
corresponding velocity. If {$\tau$} is the effective optical depth of
an absorbing cloud that occults a fraction {$C_{\rm f}$} of the source,
the observed residual intensity, $R$, in normalized
units is:
\begin{equation}
R(\lambda) = [1-C_{\rm f}(\lambda)] + C_{\rm f}(\lambda) e^{-\tau(\lambda)} \quad .
\end{equation}
The first term on the right--hand side represents the photons traveling
along unocculted lines of sight while the second term arises from
photons that survive absorption due to the finite optical depth of the
cloud.

For two multiplet transitions, the conjunction of the two residual
intensities with the optical depth scaling yields the coverage
fraction through the solution to:
\begin{equation}
\left [{{R_{\rm r}-1+C_{\rm f}} \over {C_{\rm f}}}  \right ]^{{f_{\rm b} \lambda_{\rm b}}
\over
{f_{\rm r} \lambda_{\rm r}}} = {{R_{\rm b}-1+C_{\rm f}} \over {C_{\rm f}}} \quad ,
\end{equation}
where the subscripts ``r'' and ``b'' refer to the properties of the
redder and bluer transitions, respectively.  For the resonant UV
doublets, such as {{\rm C}\kern 0.1em{\sc iv}~$\lambda\lambda 1548, 1550$}, {${{f_{\rm b} \lambda_{\rm b}} \over {f_{\rm r} \lambda_{\rm r}}} \approx 2$} allowing an analytic
solution:
\begin{equation}
C_{\rm f}(v) = {\left[R_{\rm r}(v)-1\right]^2 \over {R_{\rm b}(v)-2R_{\rm r}(v)+1}}
\quad ,
\end{equation}
where we have converted the wavelength dependence of the coverage
fraction to a velocity dependence. In the application of this method
to the data, the calculation of {$C_{\rm f}$} was performed in each
resolution element along each of the resonant doublet profiles for the
three associated systems with anomalous optical depth ratios.  The
results are illustrated as points with {$1\sigma$} error bars in the
bottom window of each panel of
Figures~\ref{fig:q0450f2}--\ref{fig:q1329f2}.  Points are only plotted
if: (1) the stronger transition is detected, using the aperture method
(Lanzetta, Turnshek, \& Wolfe 1987\nocite{ltw87}), at the $3\sigma$
level; (2) the derived coverage fraction is physical ($0 < {C_{\rm f}} <
1$); (3) the $1\sigma$ error in {$C_{\rm f}$}, $\sigma_{C_{\rm f}} < 0.5$; and (4)
the fractional uncertainty in ${C_{\rm f}}$ is less than unity.

A notable trend is that the coverage fraction always drops toward the
wings of lines. This is an effect of the instrument's line spread
function which tends to ``wash out'' the wings and artificially cause
anomalous optical depth ratios. We have explored this effect by
simulating observed spectra with normal optical depth ratios and
analyzing them in the same way as the data. As shown in
Figure~\ref{fig:inseff}, synthetic spectra which are not convolved
with the line spread function exhibit no variation in the coverage
fraction across the single component Voigt profile. When convolved
with the instrumental resolution function, even a profile with
${C_{\rm f}}=1$ will show ${C_{\rm f}}<1$ in its wings due to this convolution
effect. The signal--to--noise ratio of the observed spectra was not high
enough to merit an attempt to deconvolve the line spread function.
Therefore it is only possible to interpret the derived ${C_{\rm f}}$ values
in the cores of well--resolved lines.

There is evidence for partial coverage (${C_{\rm f}} < 1$) over a
significant range of velocity for the three systems. The values of
${C_{\rm f}}$, averaged over the velocity regions defined by the {\it
apparent} location of kinematic components in the profile, are given
in Table~\ref{tab:covfac2}.  The weighted mean values of ${C_{\rm f}}$,
averaged over all resolution elements in the regions, are also shown
graphically in the top windows of
Figures~\ref{fig:q0450f2}--\ref{fig:q1329f2}, where they are
represented by the level of the horizontal bars. The width of the
horizontal bars depicts the velocity bin over which the average value
of $C_{\rm f}$ was computed. (Note that the vertical bar does not represent
an error bar but rather it indicates the coverage fraction derived
separately for the BELR, as discussed in the next section.)

We have also found that the effective coverage fraction varies with
velocity component, as follows.  In the case of Q~$0450-132$
(Figure~\ref{fig:q0450f2}), the spectrum includes absorption lines
from three species, {\hbox{{\rm C}\kern 0.1em{\sc iv}}}, {\hbox{{\rm Si}\kern 0.1em{\sc iv}}}, and {\hbox{{\rm N}\kern 0.1em{\sc v}}}.  The coverage fraction
was derived in five separate regions of the {\hbox{{\rm C}\kern 0.1em{\sc iv}}} profile and there
is evidence that it varies from component to component.  The {\hbox{{\rm N}\kern 0.1em{\sc v}}}
data are noisy, but consistent with the coverage fraction derived for
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} in regions of overlap.  The {$\Delta v=-2100~{\rm km~s^{-1}}$}
component that shows strong {\hbox{{\rm Si}\kern 0.1em{\sc iv}}} absorption (presumably originating
from a lower--ionization region of the absorber) also shows partial
coverage consistent with the corresponding component of {\hbox{{\rm C}\kern 0.1em{\sc iv}}}.  There
are two distinct components in the PG~$1222+228$ intrinsic {\hbox{{\rm C}\kern 0.1em{\sc iv}}}
absorption profile (Figure~\ref{fig:q1222f2}), both of which yield a
small coverage fraction: the {$\Delta v=+1469$~\hbox{km~s$^{-1}$}} component gives
$C_{\rm f}\approx 0.7$ while the {$\Delta v=+1587$~\hbox{km~s$^{-1}$}} component gives
a coverage fraction of about $C_{\rm f}\approx 0.4$.  The effective coverage
fraction was also determined in four separate regions of the intrinsic
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} profile of PG~$1329+412$ (Figure~\ref{fig:q1329f2}); in two of
which we found ${C_{\rm f}}<1$.

\subsection{Partial Coverage of Continuum and Emission Line Sources}

The single number {$C_{\rm f}$} gives the fraction of all photons at a given
wavelength that pass through absorbers along the line of sight.
However, at the position of these associated absorption lines in the
spectrum, the absorbed photons have two significant sources, the
continuum source and the BELR.  The continuum source is likely to be
significantly smaller than the BELR, but the geometry and relative
position of the BELR is unknown. In this section, we continue to
assume that the photons from these two regions pass through the same
absorbers, i.e. that the optical depth $\tau$ is the same along the
paths to the observer from the continuum source and from the BELR.
However, we now consider the different coverage fractions, {$C_{\rm c}$} and
{$C_{\rm elr}$}, that can apply for the continuum source and the BELR.
First we define, $W = F_{\rm elr}/F_{\rm c}$, as the ratio of the
broad emission--line flux to the continuum flux at the wavelength of
the narrow absorption line.  Then we can write the normalized flux as:
\begin{equation}
R = 1 - {{(C_{\rm c} + W C_{\rm elr}) (1-e^{-\tau})} \over {(1+W)}} \quad .
\end{equation}
By the same optical depth scaling argument as in the previous section, this
reduces down to:
\begin{equation}
{{C_{\rm c} + W C_{\rm elr}} \over {1 + W}} = {[(R_{\rm r}(v)-1)]^2 \over
{R_{\rm b}(v)-2R_{\rm r}(v)+1}} = C_{\rm f} \quad ,
\end{equation}
where we have assumed that underlying, unabsorbed continuum plus line
flux is the same in both transitions, i.e., that the value of $W$ is
the same for both members of the doublet. In the Appendix we calculate
that {$C_{\rm c}$} or {$C_{\rm elr}$} will change by at most 15\% if a doublet is
on the steep slope of an emission line due to a differing $W$.
Equation~(5) shows that the effective coverage fraction, {$C_{\rm f}$}, can
be considered as an average coverage fraction weighted according to
the flux from each source. Of course, with the available information,
the continuum source and BELR coverage fractions cannot be determined
independently of each other. It is possible, nevertheless, to place
interesting constraints on them.  Given the value of $C_{\rm f}$ and $W$,
and their $1\sigma$ uncertainties, equation~(5) defines a region in
the $C_{\rm c}$--$C_{\rm elr}$ parameter plane where the solution must
lie. Examples of such regions are illustrated in
Figure~\ref{fig:illust}. It is interesting to note that, if the upper
boundary of this allowed region intersects one of the axes at a value
below 1, then the value of the corresponding coverage fraction must be
less than unity (at the $1\sigma$ confidence level). Such a situation
can occur if the narrow absorption doublet happens to fall on the
high--velocity wing of an emission line where the underlying flux is
dominated by the continuum (i.e., when $W$ is small). Because of this
technical requirement, we cannot draw any conclusions about the
preferred velocity distribution of systems that cover the continuum
source only partly.

Using the observed values of $W$ from published low--resolution spectra
(\cite{sbs88}; \cite{ss91}) and the measured values of $C_{\rm f}$ we have
derived constraints on the coverage fractions of the two distinct
sources. These limits, along with the ingredients needed to compute
them, are listed in Table~\ref{tab:covfac2} for each system and
transition showing the signature of partial coverage. In particular,
in the last two columns of Table~\ref{tab:covfac2} we list the range
of allowed values of {$C_{\rm c}$} and {$C_{\rm elr}$} as deduced from the range
of allowed solutions of equation~(5).  We emphasize that the limits on
{$C_{\rm c}$} and {$C_{\rm elr}$} do not hold independently of each other since
the solution should also satisfy equation~(5). In practice these
limits correspond to the extreme corners of the solution boxes as
illustrated in Figure~\ref{fig:illust}.  The constraints on {$C_{\rm c}$}
and {$C_{\rm elr}$} are also represented graphically by the vertical extent
of shaded boxes and vertical bars, respectively, in
Figures~\ref{fig:q0450f2}--\ref{fig:q1329f2}.

In most of the absorption components listed in
Table~\ref{tab:covfac2}, either the continuum source or the BELR could
be fully covered.  Notable exceptions are the {\hbox{{\rm Si}\kern 0.1em{\sc iv}}} line of
Q~$0450-132$ and the highest--velocity component of its {\hbox{{\rm N}\kern 0.1em{\sc v}}} line (at
$\Delta v=-1880$~{\hbox{km~s$^{-1}$}}; see Figure~\ref{fig:q0450f2}), as well as
the red {\hbox{{\rm C}\kern 0.1em{\sc iv}}} component in PG~$1222+228$ (at $\Delta v=+1587$~{\hbox{km~s$^{-1}$}};
see Figure~\ref{fig:q1222f2}).  In these cases {$C_{\rm elr}$} is not
constrained, but the continuum source cannot be fully covered under
any conditions. We derive $0.59 < {C_{\rm c}} < 0.88$ and ${C_{\rm c}} < 0.84$,
respectively, in the case the former object and $0.12 < {C_{\rm c}} < 0.52$
in the case of the latter object. In the Appendix we consider the
possibility that the photons from the continuum source and the BELR
pass through different absorbers, i.e. $\tau_c \ne \tau_{elr}$.  This
could be possible depending on the sizes of absorbing structures and
their spatial positions relative to the emitting regions, but we show
in the case of the redward component of PG~$1222+228$ partial coverage
of the continuum source is required regardless of the assumed $\tau_c$
and $\tau_{elr}$.  The $\Delta v=+1587$~{\hbox{km~s$^{-1}$}} component of the
PG~$1222+228$ system also requires a partially covered continuum
source, with a larger continuum coverage fraction. It is interesting
that the range of constraints $0.51 < C_{\rm c} < 0.92$ does not overlap
with that of the $\Delta v=+1469$~{\hbox{km~s$^{-1}$}} component.

\subsection{Application of the Refined Method to Additional Quasars With
Published Data}

There are three other quasars with intrinsic {\hbox{{\rm C}\kern 0.1em{\sc iv}}} narrow line
absorbers observed with HIRES/Keck~I and presented in the literature
in sufficient detail to derive {$C_{\rm f}$}, {$C_{\rm c}$}, and {$C_{\rm elr}$}.  These
are PKS~$0123+237$ (radio--loud; \cite{bs97}), Q~$0150-203$ (UM 675;
radio--quiet; \cite{ham97a}), and Q~$2343+125$ (radio--quiet;
\cite{ham97b}). The results we obtain by applying the method of the
previous section to these objects are listed in Table~\ref{tab:covfac}.

The NAL systems of PKS~$0123+237$ were discussed by Barlow and Sargent
(1997\nocite{bs97}).  The velocity structure of
the NAL profile of PKS~$0123+237$ is similar to that of Q~$0450-132$
but in the former object the effective coverage fraction is different
for different transitions. In the case of Q~$2343+125$ (\cite{ham97b})
the NALs are found at a very large velocity relative to the
emission--line peak ($\Delta v=-24,000$~{\hbox{km~s$^{-1}$}}) but still there is
considerable evidence that they are intrinsic: in addition to showing
the signature of partial coverage they also happen to be variable.
The continuum coverage fraction can be constrained to be very small
($<0.2$) because the emission--line contribution at the velocity of
absorption is small ($W = 0.1$; see Table~\ref{tab:covfac}).

Together with the NAL systems presented in the previous section, the
systems analyzed here comprise the database of available
high--resolution spectra of NALs.  All six intrinsic NAL systems have
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} absorption profiles with velocity widths of $100$--$400$~{\hbox{km~s$^{-1}$}}
and have obvious sub--structure (see, for example,
Figure~\ref{fig:q0450f1}).  The NAL profiles suggest that there are
discrete absorbing structures (though not necessarily discrete
``clouds'') at different positions in velocity space.

\section{Discussion}

\subsection{Implications of the Observational Results}

Since the six quasars of Table~\ref{tab:qso} were drawn from a sample
that was selected based on the properties of {\it intervening} {\hbox{{\rm Mg}\kern 0.1em{\sc ii}}}
absorbers, they can be regarded as a collection which is unbiased
towards the detection of {\it associated} {\hbox{{\rm C}\kern 0.1em{\sc iv}}} absorption lines. As
such we can use it to estimate roughly how frequently associated
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} NALs are found in radio--loud and radio--quiet quasars.
Associated absorption lines were detected in all three radio--quiet
objects, and, in two cases, the lines were shown to be intrinsic based
on the signature of partial coverage. The two NAL systems in
Q~$1213-003$, which did not show the signature of partial coverage,
could plausibly be intervening. One would expect to find 2 intervening
systems within 5000~{\hbox{km~s$^{-1}$}} in a sample of six quasars, based on the
known density of {\hbox{{\rm C}\kern 0.1em{\sc iv}}} systems at $z=2$ and the redshift path that we
have observed.  On the other hand, only one out of the three
radio--loud objects showed an associated NAL system which also turned
out to be intrinsic.

Our results are consistent with previous studies
(\cite{foltz86}; \cite{and87}) that find that associated NALs
are fairly common in both radio--loud and radio--quiet quasars.
However, as Foltz {et~al.}~(1986\nocite{foltz86}) pointed out, there
could be a systematic difference between the strengths of associated
NALs found in radio--loud and radio--quiet quasars.  Strong
NALs ($>1.5$~{\AA}) prefer radio--loud hosts, while weak NALs show
no such preference.  None of the five associated systems detected
in our survey are strong, thus we cannot re--address this issue.
It should be noted that although the associated systems
that we report here are fairly weak, in three our of four quasars they
are still within the detection limits of the
Foltz {et~al.}~(1986\nocite{foltz86}) and Anderson {et~al.}~(1987) surveys.
However, our more sensitive survey shows that in some cases
(Q~$0002+051$ and Q~$1421+331$) NALs are {\it not} detected down to
a $5\sigma$ limit of rest--frame equivalent width, $REW < 0.05$~{\AA}.
This implies that there
may be some lines of sight that do not pass through NAL gas.

More than 10 intrinsic NAL systems reported in
the literature appear in radio--quiet quasars (\cite{ham97c};
\cite{bhs97}; Tripp, Lu, \& Savage 1997\nocite{tripp}). It is
interesting that, although Foltz {et~al.}~(1986\nocite{foltz86}) and
Anderson {et~al.}~(1987\nocite{and87}) find associated NALs in about 70\%
of radio--loud quasars, only very few of these systems have been proven
rigorously to be intrinsic: two systems from the sample of Foltz
{et~al.}~(1986) show signs of variability (3C~$205$ and the ``mini--BAL''
in PHL~$1157+0128$; \cite{ald97}). Moreover, some fraction of
associated NAL systems are bound to be intervening systems by chance;
in fact 2 out of the 12 associated NAL systems in the sample of Anderson
{et~al.}~(1987\nocite{and87}) are expected {\it a priori} to be
intervening systems.
A description of the properties of {\it intrinsic} NALs in
radio--loud and radio--quiet quasars
has not yet been established.  A systematic survey at very high
spectral resolution is needed to clarify the situation.

Another important observational result is that, in at least two
quasars from our collection, the NAL gas can be demonstrated to cover
the {\it continuum source} only partially. One of these quasars,
Q~$0450-132$, is radio--quiet, while the other, PG~$1222+228$, is
radio--loud. Partial coverage of the continuum source may be more
common than these two cases suggest but we have no way of determining
this yet.  The implication of this result is not absolutely clear
because the reason for the apparent partial coverage is not known. One
possibility is that the absorbing medium is clumpy and the clump sizes
are comparable to or smaller than the size of the continuum
source. Another possibility, however, is that the continuum source is
completely covered by the absorber but a scattering medium makes it
possible for continuum photons to bypass the absorber and get to the
observer without suffering any absorption. We expand on this issue in
the next section where we consider possible explanations for the
observed partial coverage.

\subsection{Interpretation of Effective Partial Coverage}

Central to interpreting these results is knowledge of the mechanism
that can give rise to effective coverage fractions less than unity.
Following our preliminary discussion of this subject in \S3, three
mechanisms can fill in saturated, non--black troughs, or more generally
produce discrepant optical depth ratios for doublet or multiplet
transitions: 1) a source function, 2) scattering of background photons
back into the light path, 3) true (i.e., geometric) partial coverage
of the continuum and/or BEL source by the absorbing medium.  The
present data do not permit us to distinguish among these
possibilities, but we discuss possible tests.  These tests involve
polarization measurements, consideration of the coverage fraction in
different transitions, and correlating time variability with coverage
fractions.

One possible source function explanation involves a non--occulted
emission source which contributes additional photons to the light path
after absorption of the continuum and BEL photons has occurred,
essentially ``diluting'' the absorbed spectrum. Wampler
{et~al.}~(1995\nocite{wam0059})
determined that an unabsorbed thermal continuum characterized by
$T=17,000$~K could explain the residual intensity in the saturated
troughs of various transitions in the BAL system of Q~$0059-2735$. In
fact, other intrinsic NAL systems also show variations in $C_{\rm f}$ from
transition to transition, namely UM675 (\cite{ham97a}) and
PKS~$0123+257$ (\cite{bs97}). The mechanism for production of the
additional source function photons is unknown, but its contribution
should vary smoothly with wavelength to produce the observed
effect. Another manifestation of a source function is line emission by
the same gas that is responsible for the absorption. This version of
the scenario is not viable, however, since it would not have the
desired effect: if there were an emission component filling in the
unresolved absorption troughs it would result in an effective coverage
fraction {\it greater that unity}.

Scattering of photons back into the light path is certainly a
plausible explanation.  An indirect argument for a scattering
explanation is that it is known to be important in filling in the
troughs of {\it broad} absorption lines. Spectropolarimetric
observations of many BAL quasars (\cite{ogle97}; \cite{broth97};
\cite{cohen95}; Glenn, Schmidt, \& Foltz 1994\nocite{glenn94};
\cite{good95}; \cite{hines95}; \cite{schmidt97}) show that the
polarization level in saturated non--black absorption troughs is higher
than in the continuum.  This by no means proves that scattered light
makes a large contribution for all NAL absorbers, since the lines of
sight through these absorbers could well be different than in
BALs. Spectropolarimetric observations of partially covered NAL
systems are needed to investigate the role of scattering.  Until such
observations are carried out, we can consider clues provided by the
relationship between time variability and partial coverage. The
implications of the observational clues, however, depend on the
picture that one adopts for the scatterers. If the scatterers comprise
an extended collection of clumps or a quasi--uniform medium enveloping
the BELR, then the scattering contribution is unlikely to vary
substantially over time scales of the order of the dynamical time of
the BELR gas. The strength of absorption, on the other hand, can vary
as a result of changes in ionization state of the absorber or motion
of the absorbing gas across the line of sight. One alternative picture
is that of a discrete clump acting as a mirror to scatter continuum
and/or emission--line photons in the direction of the observer without
their passing through the absorber.  In this picture the amount of
scattered light can vary on the same time scale as the absorbing
column density making a unique interpretation of the variability time
scale virtually impossible. Another alternative picture is that the
scatterers are close to our line of sight (they could be mixed with
the absorbers or they could form a tenuous, ionized atmosphere round
individual clumps in the absorber). In this case the light is
scattered in the forward direction and its fractional polarization
does not change. In other words, even though scattering is the culprit
in this scenario, it does not betray itself by its polarization
signature.

At present there is one NAL system where variability provides strong
evidence {\it against} a scattering mechanism. The $\Delta
v=-24,000$~{\hbox{km~s$^{-1}$}} {\hbox{{\rm C}\kern 0.1em{\sc iv}}} NAL system toward Q~$2343+125$ has an
effective coverage fraction that varies substantially from one epoch
of observation to another, and the effective coverage fraction is
smaller when the absorption lines are weaker (\cite{ham97a}). This
argues against a scattering picture of the above type, in which
scattered light would fill in a larger fraction of the trough of a
weaker line.  From the time variability and the partial coverage of
the continuum source for this system, Hamann {{et~al.}} (1997b) derived
the requirement that the absorbing clouds are quite small ($\sim
0.01$~{\rm pc}) and are located close to the continuum source. If we
adopt this interpretation, then true partial coverage of the continuum
source is the most plausible explanation. This suggests that time
variability and true partial coverage occur together because both are
related to small absorbers close to the continuum and/or BEL source.
The variations can result from either motion of the clouds or from
changes in the sizes of the multiphase layers of the absorber.
Discriminating between these two possibilities is challenging and
requires a geometric model of the absorbers and the sources of
ionization, which can be constrained by observations of multiple
transitions.

\subsection{A General Picture of Intrinsic NALs}

Narrow absorption lines are ubiquitous, appearing in all types of
broad--line AGNs, namely in Seyfert~1 galaxies and broad--line
radio galaxies as well as in radio--loud
and radio--quiet quasars. If we take the frequency of narrow {\it
associated} absorption lines as a rough indication of the coverage
fraction of the absorbers (as seen by the continuum and/or
emission--line source) then this fraction appears to be very high. It
is about 50\% in Seyfert~1 galaxies (Crenshaw 1997), perhaps about
70\% in radio--loud quasars (Foltz {et~al.}~1986; Anderson {et~al.}~1987),
and apparently also very high in radio--quiet quasars based on our small
collection.

The observational clues available at the moment, although tantalizing,
do not point clearly to a specific interpretation. Because NALs are
seen in many different types of active galaxies and seem to be quite
common, their relation to BALs is unclear.  Unlike BALs, NALs are
common in radio--loud quasars and in Seyfert 1's. It is plausible that
NALs with large velocities and those that are quite broad and without
structure (``mini--BALs'') are related to the BAL phenomenon
(\cite{ham97c}). This hypothesis is supported by the fact that large
outflow velocities ($>$10,000~{\hbox{km~s$^{-1}$}}), such as in Q~$2343+125$,
Q~$0935+417$ (\cite{ham97c}), and Q~$1700+64$ (\cite{tripp}), have
only been observed in radio--quiet quasars, as have the majority of
BALs. Radio--loud quasars on the other hand have mostly narrow,
``associated'' absorption lines.  Finally, associated NALs found in
Seyfert~1 galaxies show limited observational evidence for an
intrinsic nature. Some have covering factors close to unity
(\cite{cren97}), and in two cases, NGC~3783 and NGC~3516, the NALs
vary on a short time scale (\cite{korat96}; \cite{shields97}).
Interestingly enough NALs in Seyfert~1 galaxies are always blueshifted
relative to the BELs, unlike NALs in quasars which are sometimes
redshifted relative to the BELs. Based on the above summary, a
reasonable model or scenario for the NAL gas should explain why NALs
are so common (in other words, why the absorbing gas covers such a
large solid angle relative to the continuum source) and why they are
sometimes observed to be redshifted and sometimes blueshifted relative
to the peaks of the broad emission lines (i.e. apparent infall
as well as outflow).

It is obviously impossible to construct a unique unifying model to
explain these observational facts.  Nevertheless, we venture to
speculate on how NALs can fit into the accretion--disk wind picture of
Murray {{et~al.}} (1995\nocite{mur95}), which was originally meant to
explain BALs. Their possible relatives, the high velocity NALs, could
originate in a different phase of the same region or in an atmosphere
just outside the wind.  Sometimes both NALs and BALs arise in the same
quasar, at different velocities, so it seems plausible that NAL phases
could exist nearby the BAL region.  The broader, smoother, mini--BALs
may also be related to this type of wind flow. In this context, it is
extremely interesting that in some cases the NALs are redshifted
relative to the {\it broad} emission--line peak. Of course this
relative redshift does not necessarily imply infall towards the
central engine. The systemic redshift is best determined from the {\it
narrow} emission lines, which, however, have not been observed in
these particular objects. Because the peaks of the broad emission
lines can be blueshifted relative to the systemic redshift, it is
possible that the observed NALs are also blueshifted relative to the
systemic redshift.  At any rate, all four of the NAL systems in
radio--loud quasars that have been demonstrated to be intrinsic, i.e.,
PG~$1222+228$ (this paper), Q~$0123+237$ (\cite{bs97}), $3$C~$205$
(\cite{ald97}), and PHL~$1157+014$ (\cite{ald97}), have NALs that {\it
appear to be} redshifted with respect to the peaks of the broad
emission lines.  In Figure~\ref{fig:cartoon}, we show schematically a
side view of the geometry of the accretion--disk wind of Murray {{et~al.}}
(1995) and a plausible location for the NAL gas.  For specific
orientations of the observer (such that $\beta < i$, where $i$ is the
inclination of the disk relative to the observer and $\beta$ is the
opening angle of the wind,
as shown in the figure), the NALs originating in the far side of the
disk can appear redshifted, assuming that the NAL gas is outflowing.
Since the NALs are sometimes deeper than the net emission--line level
on which they are superposed, the absorbing gas must intercept
continuum photons as well. To accommodate such an effect in this
picture we must postulate that the outflowing NAL gas originates very
close to the center of the disk so that it can cover the continuum
source, i.e., it fills the region between the fast disk wind
and the disk axis. We emphasize, however, that alternative
pictures are also plausible. For example, the NAL gas could be located
on the near side of the disk, in the direction of the
observer. Because the wind is rotating as well as outflowing, the net
velocity vector of the outflowing gas can point away from the observer
depending on the azimuth, in which case the resulting absorption lines
will also appear redshifted.

In the context of the speculative geometric picture outlined above,
the difference between AGN subclasses may be related to the properties
of the fast wind. For example, if the opening angle of the wind is
very small, the wind effectively ``hugs'' the accretion disk and the
likelihood of our line of sight going through it is very small. Hence
BALs would not be observed in such objects but NALs could still
appear. We speculate further that the difference between
radio--quiet quasars on one hand and radio--loud quasars and Seyferts on
the other is the opening angle of the wind, which may in turn be a
consequence of the luminosity of the object (relative to the
Eddington luminosity), of the shape of the ionizing continuum, or
of the combination of these two properties.
This could also affect the strength of NALs in the two cases as
observed by Foltz {et~al.}~(1986) for radio--loud vs. radio quiet quasars.
Finally, we note that if any hot electrons happen to be located in the
direction of the axis of the disk, they can act as scatterers and
redirect continuum photons towards the observer. Through this effect,
the absorption lines can be ``diluted'' creating the impression that
the absorber only partly covers the continuum source.

\section{Summary and Conclusions}

In this paper we reported the discovery of five narrow ``associated''
($\vert\Delta v\vert<5000$~{\hbox{km~s$^{-1}$}}) absorption--line systems in the
spectra of four quasars. These quasars were observed in the course of
a survey for intervening {\hbox{{\rm Mg}\kern 0.1em{\sc ii}}} absorbers, in which the {\hbox{{\rm C}\kern 0.1em{\sc iv}}}
emission lines of six objects happened to fall in the observed
spectral range.  As such, this ``mini--sample'' of six quasars is
unbiased towards the presence of narrow, intrinsic {\hbox{{\rm C}\kern 0.1em{\sc iv}}} absorption
lines.  Three of the absorption systems were demonstrated to be
intrinsic, because the relative strengths of the members of the
{\hbox{{\rm C}\kern 0.1em{\sc iv}}} doublet required effective partial coverage of the continuum
and/or emission--line sources. The two systems toward Q~$1213-003$
could not be demonstrated as intrinsic because their coverage
fractions were consistent with unity.

We carried out a detailed analysis of the coverage fractions of the
three intrinsic systems that we have found: Q~$0450-132$,
PG~$1222+228$, and PG~$1329+412$. The analysis consisted of
determining the effective coverage fraction of the background
source(s) by the absorber according to the method of Barlow \& Sargent
(1997\nocite{bs97}) as well as a refinement of this method to treat
the coverage fractions of the background continuum and emission--line
sources separately. The latter technique was also applied to three
additional intrinsic NAL systems for which sufficient information was
available in the literature: PKS~$0123+237$, UM~$675$, and
Q~$2343+125$.  This provided a total of six intrinsic NAL systems
studied at high resolution, and among the six there was a very wide
range of properties.  The derived {\hbox{{\rm C}\kern 0.1em{\sc iv}}} effective coverage fractions
ranged from $C_{\rm f} \sim 0.1$ to nearly unity, and in some systems varied
across the absorption profiles.  The velocities of the absorbing
clouds, relative to the quasar, ranged from outflow at $24,000$~{\hbox{km~s$^{-1}$}}
to apparent infall at $1500$~{\hbox{km~s$^{-1}$}}.  In three systems, Q~$0450-132$
and PG~$1222+228$ (this study) and Q~$2343+125$ (\cite{ham97b}), the
data require that the covering factor of the {\it continuum} source is
less than unity ($C_{\rm c} < 1$, according to our formulation presented in
\S4.2).  The two systems are quite different from each other:
Q~$2343+125$ is radio--quiet and its absorption system is at an outflow
velocity of $24,000$~{\hbox{km~s$^{-1}$}}, while PG~$1222+228$ is radio--loud and its
absorption system is redshifted relative to the BEL region by
$1500$~{\hbox{km~s$^{-1}$}}.

We have discussed mechanisms which can give rise to a covering factor
that is less than unity but we have not been able to select a favorite
based on the information that is currently available from
observations. We have also speculated that the NAL gas may be related
to the fast outflows that manifest themselves as BALs.  If this is
indeed the case, then the fact that NALs are quite common in radio--loud
quasars and in Seyfert~1 galaxies may imply that these types of AGN
also harbor fast accretion--disk winds, whose absorption signature
(BAL) is unobservable. Further observations, and more specifically
systematic surveys of the various classes of active galaxies and
quasars, are needed to test these ideas.  Some of the key goals of
these surveys should be to: 1) establish just how common {\it
intrinsic} NALs are in radio--loud/quiet quasars and in Seyfert 1's; and
2) check if non--unity covering factor and time variability
occur together as a clue toward understanding the spatial distribution
of the NAL clouds. In addition spectropolarimetric observations are
sorely needed to establish whether scattering or true partial coverage
by small absorbers is responsible for effective covering factors less
than unity.

\acknowledgments

We thank Jules Halpern as well as the anonymous referee for useful
suggestions.  This work was supported by the National Science
Foundation Grants AST--9529242 and AST--9617185, and by NASA Grant
NAG5--6399.  During the early stages of this work M.E. was based at the
University of California, Berkeley and was supported by a Hubble
Fellowship (grant HF--01068.01--94A from Space Telescope Science
Institute, which is operated for NASA by the Association of
Universities for Research in Astronomy, Inc., under contract
NAS~5--26255). We are grateful to Steven S. Vogt for the great job he
did building HIRES.

\section*{APPENDIX}

redpajama_set_name: RedPajamaArXiv


Scientists are making their first forays into the mysterious world of microbes living thousands of metres in the air. Their startling conclusion: That ecosystems in the sky might influence much of the world's weather, including snowfall.
The plane pitches violently as it plows through the milky innards of a cloud bank. A commercial pilot would fly high above these clouds over California's Sierra Nevada Range, but this 20-metre Gulfstream-1 seems to invite the turbulence. Updrafts grab hold of the aircraft and shove it up even as the pilot noses it down. In the back of the plane, atmospheric chemist Kimberly Prather wears headphones to muffle the roar of the propellers. She steadies herself with a hand on an instrument rack and focuses on the bobbing screen of her laptop. Readings from the clouds spool across it.
Those numbers tell Prather that these winter clouds are cold and heavy, –30 degrees Fahrenheit and just over 100 per cent relative humidity. Yet despite being 62 degrees below the freezing point of water, the cloud droplets remain stubbornly liquid. As long as they don't form ice crystals, these clouds won't shed more than a few flakes of snow over the Sierras' 4,000-metre peaks. They are typical clouds, teasers that won't drop much of anything.
After two hou rs of flying, though, something changes. The voice of another researcher crackles over Prather's headset: "Ice!" The plane has entered a cloud layer where suddenly every droplet is frozen. Prather's instrument — a tangle of metal tubes, wires, and airtight chambers nicknamed Shirley — tick-tick-ticks as its laser blasts apart hundreds of microscopic cloud particles, one by one, that are drawn in from the air outside. The size and composition of each particle flash across Prather's monitor. The specks at the heart of those ice crystals are high in aluminum, iron, silicon, and titanium, the chemical signatures of dust not from California but from faraway deserts in Asia or even Africa. There's something else in the crystals too: carbon, nitrogen, and phosphorus, telltale signs of biological cells.
The skies are full of invisible life. Bacteria, algae, and fungi are swept up by winds and lifted to the altitude of a Boeing 747 — or catapulted 30 kilometres into the stratosphere by electric fields during thunderstorms. Prather, a 49-year-old professor at the University of California, San Diego, is one of a growing number of scientists who suspect this largely unexplored microbial ecosystem might hold the answer to one of the great mysteries of the weather: Why do clouds produce precipitation when they do?
It seems like such a basic question, but "we really don't understand why some clouds drop rain and others don't," Prather says. At the heart of this mystery is the physics of ice formation. A pure cloud droplet can cool to –36.4ºF before it freezes, and many clouds on Earth never get anywhere near this cold. Rain and snow often require tiny particles floating in the cloud to trigger ice to form, and not just any particle will do. A cubic yard of air contains hundreds of thousands of microscopic specks, but only about one in a million possesses the exact molecular geometry that will organize water molecules on its surface to spawn an ice crystal. Without those rare ice-forming triggers, much of the planet would see less precipitation than it does today.


Stuck at home in bed, got an assignment due and not feeling your best? But know you have to get on with it? Looking after the kids in the park at assessment crunch time?
Kathryn has talked to students in many situations like these, including whispered conversations while babies are sleeping.
We know everyone gets busy and that adds to rising stress levels at crucial times in term. And when time is not on your side, using the Library more effectively can make a big difference. Peer-reviewed articles, date ranges and online and available now? There is a lot of information out there; great search skills can keep you on track and save time!
Kathryn loves working alongside students just like you, helping cut through the confusion and reducing stress. She understands the balancing act of studying and working, and the uncertainty that all students can feel.
Lock in an appointment with a librarian like Kathryn and learn skills for your assessment, and your future educational journey.
Studying by online education can be an isolating experience. It is hard to know how to get started, where to turn for help or even what the question is! As a distance student himself, John understands that you really need encouragement and support – a little virtual cheer squad at your side!
Maybe you feel like your question is silly or you should know the answer. Maybe even getting started seems impossible. Or are you further down the track in your assessment, but looking for that awesome reference to impress your lecturer and smash those great marks? Librarians are there for you – to help you understand your assessment question, evaluate sources and refine your search.
Accessing assistance from John and our team of online librarians is as easy as picking up your phone or logging in to your computer! And with the option of our Ask a Librarian video sessions, it can be a great personal, online face-to-face experience.
Choose a time on our Ask a Librarian calendar!
Want to know more about the library and IT at CQUni? Check out our quick guide.


text:
Ruling can't keep Rob Ford off football field
Toronto Mayor Rob Ford speaks at city hall on Nov. 26, 2012. Mr. Ford was ordered removed from office on Monday after a judge found him guilty of breaking conflict-of-interest laws.
MARK BLINCH/REUTERS
Jeff GrayQueen's Park Reporter
Karen Howlett
David Shoalts
Published November 26, 2012 Updated May 9, 2018
Mayor Rob Ford's political troubles could not keep him away from the football field, especially on the eve of his team's first-ever run at the Toronto region's high school equivalent of the Grey Cup.
It is a championship bid 10 years in the making, since Mr. Ford took the reins of the football program at Don Bosco Catholic Secondary School in 2002 as a volunteer coach. Wrapped in a hoodie, the mayor led the team through the last 45 minutes of a final practice on Monday ahead of the championship game in the Metro Bowl at the Rogers Centre on Tuesday. The mayor is expected to be there even if meetings at City Hall, where his leadership is in doubt, go into overtime.
His love for football and the young players he mentors got him into this legal quandary – and a $3,150 donation from lobbyists and their clients to his football foundation.
But it was Ontario's Municipal Conflict of Interest Act, and its ironclad penalties that led to a judge's order that he leave office in 14 days.
The legislation, which Mr. Justice Charles Hackland of the Ontario Superior Court called a "very blunt instrument" as he made his ruling, has often been criticized by lawyers; the province is currently reviewing it.
The act gave Judge Hackland only two options once he determined that Mr. Ford had violated it, and not "inadvertently" or through an "error in judgment": ordering him out of office and banning him from running for up to seven years. Judge Hackland declined to bring the second penalty down on Mr. Ford's head. Mr. Ford, the judge ruled, did not deserve such a sanction because he was not involved in an issue of "corruption or pecuniary gain."
A spokeswoman for Bob Chiarelli, the province's Minister of Municipal Affairs, said on Monday the legislation is under review, as well as another major law that governs local politicians, the Ontario Municipal Act. The conflict-of-interest act's strict penalties stand in stark contrast to the latter, under which sitting councillors and mayors may not be forced from office even if they are convicted of a crime. Mayors or members of council can lose their posts under this law only if they are actually incarcerated.
The difference is illustrated by a controversy in London, Ont., where mayor Joe Fontana has refused to step down despite facing criminal fraud charges. Unlike Mr. Ford, the London mayor, who denies the allegations, has not been found by a judge to have violated any law.
"The good fortune that Mr. Fontana has is that he is not alleged to have broken the Conflict-of-Interest Act," said Myer Siemiatycki, a political science professor at Ryerson University.
Premier Dalton McGuinty, who offered little comment about the ruling against Mr. Ford other than that it was "surprising," declined to say whether the penalties in the Conflict of Interest Act are too harsh, or whether his government should make it a priority to review the legislation. "There's nothing that strikes me of an emergency nature here," he told reporters.
Mr. Ford got a much more sympathetic reception from the Official Opposition at Queen's Park. "I think it's tragic when a political figure winds up in a position like this," Progressive Conservative MPP Peter Shurman said. "He has done a reasonably good job in our estimation of handling affairs at the City of Toronto, keeping costs in check, but he has some troubles which will have to be resolved. I don't think there's anything to celebrate here."
Michael Barrack, a lawyer with Thornton Grout Finnigan LLP who was involved in a conflict-of-interest inquiry in Mississauga, Ont., two years ago, argues that allowing judges more leeway under the conflict-of-interest law would make it easier to hold politicians who repeatedly violate rules to account, not harder.
Cases involving less-severe allegations could be brought forward more often, and at less expense, he argued, because the stakes would not be as high: "That way, a guy like Ford may actually get his wrist slapped more often and that may have a greater effect at the polls because you wouldn't have to climb this very high hill to point out every time he misbehaves."
But John Mascarin, a lawyer with Aird & Berlis LLP who advises municipal politicians on conflict rules, said the act is strict for a reason: to keep any hint of personal financial gain out of municipal politics. "It is supposed to be very unforgiving. It is supposed to be a very harsh act," he said.
Mr. Ford's actions, Judge Hackland noted, were not for his own gain.
John Yan, a spokesman for the Toronto Catholic School Board, noted the amount of volunteer work Mr. Ford put into the football program, noting that it is the first appearance in the Metro Bowl for a team from the Catholic board.
"He's spent 10 years on this," Mr. Yan said at Monday's practice. "I don't think he's going to stop now."
Toronto Mayor Rob Ford vows to fight on as power scramble erupts at City Hall
A quick look back at the Rob Ford saga
Marcus Gee: Rob Ford's self-inflicted downfall
Booting Toronto's mayor wasn't 'judicial activism.' Letting him stay would have been
React: What's your take on Toronto Mayor Rob Ford's ouster?
Recap: Toronto Mayor Rob Ford testifies in libel trial
Do Rob Ford's Don Bosco students need saving? It's complicated
Judge asks if Ford's remarks went 'too far'
Council's closed-door session in dispute as Ford case falls to judge
Mayor Ford's police-board nominee draws ire
Judge rules on Ford's conflict-of-interest case on Monday
Recap: Toronto Mayor Rob Ford removed from office
Follow Jeff Gray, Karen Howlett and David Shoalts on Twitter @jeffreybgray @kahowlett @dshoalts

redpajama_set_name: RedPajamaCommonCrawl


Clermont, Georgia is the 10,517th largest city in the United States as of 2017.
Clermont, Georgia is a town.
Clermont, Georgia is as large as it has ever been. In 2017 Clermont had its largest population ever.
Clermont, Georgia is growing extremely quickly. It is growing faster than 96% of similarly sized cities since 2000.


China tech...the largest companies you've never heard of?
Today's China no longer matches the traditional view of the country. And nowhere is this more the case than in China's burgeoning technology sector. But does the trend have further to run?
Despite slowing overall GDP growth, a dramatic shift in the underlying mix of goods and services of unprecedented proportions is underway in China. Accessing the right sectors and companies is therefore crucial, as the world's second largest economy transitions to the next era.
With a middle class that has already grown to the size of America's, the scale of change in China is often underappreciated. This rising middle class is more demanding of instant service and is geared towards a digital economy. There are many instances where China has developed an ecosystem that can rival that of America's. For more analysis on this rising theme, the sector implications, and broader Asian demographic change, please see our recent Long-term Thinking articles on China and Asia.
The technology sector is an excellent case in point. China has its own equivalent of Google, Facebook and Amazon. These are Baidu, Tencent and Alibaba. Each of these companies has a similar level of market value, or capitalisation (cap), which is in excess of $500 billion (compared to the combined market cap of all FTSE 100 companies at $2 trillion). Each caters to a much larger addressable market of close to 1.4 billion Chinese. Furthermore, their reach is spreading to surrounding regions in Asia.
During the initial phases of a technological revolution in China, the Chinese government protected their local market, preventing Google, Facebook, Amazon and other US tech giants from accessing the Chinese market, thereby allowing local players to catch up. Today, each of the Chinese mega-cap companies have developed their own strongholds in China and may rival and surpass their Western competitors. These companies specialise in everything from online shopping, cloud computing, instant messaging, social media, artificial intelligence, ride-hailing apps and even autonomous vehicles.
In an environment of rising income levels, over 800 million smartphones (four times the number in the US) and openness towards technology adoption, these technology companies have are helping to drive the next leg of growth in the Chinese economy.
As an example, most people in major Chinese cities use a smartphone to pay for most things. At restaurants, a waiter will ask if you want to use WeChat or Alipay — the two smartphone payment options — before bringing up cash as a third, remote possibility. Just as startling is how quickly the transition has happened. Only three years ago there would be no question at all, because everyone was still using cash.
In 2016, China's mobile payments hit US$5.5 trillion, roughly 50 times the size of America's $112 billion market, according to consulting firm iResearch. While Tencent does not break out what it makes from mobile payments, in the fourth quarter of 2016, the 'other services' item in its earnings almost tripled from a year earlier to 6.4 billion renminbi, or US$940 million, driven largely by mobile payments.
Although each of these metrics have developed rapidly, multiplying several-fold just in the last couple of years, we believe there is still a tremendous way to go as China's affluent class moves ever more online, doing everything from shopping, to payments, to booking trips, entertainment and much more. Investors should watch this space.
Shaunak Mazumder is a Global Equities Fund Manager at LGIM, focusing on understanding long-term themes impacting global industries and companies. His specialisms include technology, telecoms, autos and consumer sectors. Shaunak joined LGIM from a multi-billion dollar fundamental focused long/short equity Hedge Fund in New York.
History suggests that equities struggle to make gains ahead of US mid-term elections. With anti-trade rhetoric likely to feature in this autumn's campaign, this time is unlikely to be different. On the other hand, we have also learnt to be prepared for the opposite with President Trump.


A good quality costume with lot of gold braid. Includes jacket, trousers and hat. 2 available in sizes 42" ~ 44" chest and 46" chest.
A good quality costume with lot of gold braid.
Includes jacket, trousers and hat.
2 available in sizes 42" ~ 44" chest and 46" chest.


Boomi has a pub, community hall, school, tennis club with five all weather courts and a pool and hot spa complex. Although small (pop. 75) Boomi has a vibrant and energetic community. The town hosts several annual tennis tournaments and has a summer competition. The tennis club is air conditioned and is utilised by community groups including the mobile preschool one day a week. The Boomi cricket team were champions in 2007. A campdraft is held annually at the end of July at the old racecourse on the outskirts of town.
Boomi also has an amateur thespian society (BATS) who stage a locally written production. This is held every two years at the end of August and is attended by approx. 700 people over four nights. It is well worth attending and guests travel from throughout the district and beyond to attend. Profits from the production assist local community groups.
The school was first established in 1901 (see history of school) with the current school being built in the early 1960's. These photographs show different views of the school.
If you know of a local education venue that servicesthis community but is not listed here, please Email us (using the button at the bottom of this page) and let us know the details, including the community to which you are referring.
LOCATION Aproximately 100Km to the northwest of Moree, just south of the Queensland border.
If your Community Organisation, Entertainment Venue or Place of Education is not listed on this site, please advise us so it can be included. If you have a web site, please advise us of the address so we can link you in.


text:
Opioid epidemic focus of June 27 Student-Invited Pharmacology Forum
Jun. 14, 2018, 8:35 AM
"America's Opioid Epidemic" is the theme of the 27th annual Joel G. Hardman Student-Invited Pharmacology Forum, beginning at 9 a.m. Wednesday, June 27, in the Vanderbilt Student Life Center.
Tennessee Attorney General Herbert Slatery III will participate in an afternoon breakout session on opioid policy with Stephen Patrick, MD, MPH, MS, director of the Vanderbilt Center for Child Health Policy and an expert on neonatal abstinence syndrome.
For a complete schedule and to register, pull down the Department Events menu on the Pharmacology Department website and click on the Student-Invited Pharmacology Forum.
Stephen Loyd, MD, medical director of the JourneyPure at the River addiction treatment program in Murfreesboro, Tennessee, and former medical director of Substance Abuse Services for the State of Tennessee;
Laura Bohn, PhD, professor of Molecular Medicine and Neuroscience at the Scripps Research Institute in Jupiter, Florida; and
Rob Gereau, PhD, director of the Washington University Pain Center, and Jose Moron-Concepcion, PhD, associate professor of Anesthesiology at the Washington University School of Medicine in St. Louis.
Vanderbilt participants in an afternoon breakout session on alternative therapies and addiction research include Erin Calipari, PhD, and Carrie Jones, PhD, assistant professors of Pharmacology; and Danny Winder, PhD, director of the Vanderbilt Center for Addiction Research.
Another breakout session on clinical intervention will feature A.J. Reid Finlayson, MD, medical director, Vanderbilt Comprehensive Assessment Program; Tracy Jackson, MD, associate professor of Anesthesiology; Hilary Tindle, MD, MPH, founding director, Vanderbilt Center for Tobacco, Addiction and Lifestyle; and Jessica Young, MD, assistant professor of Obstetrics and Gynecology.
Other participants in the opioid policy breakout session include Kevin Eidson, PharmD, a member of the Tennessee Board of Pharmacy and assistant professor in the Lipscomb University College of Pharmacy; and Andrew Finch, PhD, a national leader in recovery high schools at Vanderbilt University's Peabody College.
Following the talks, the 2018 Pharmacology Teacher of the Year award will be presented by the Pharmacology graduate students. The forum will conclude at 3 p.m. with a poster session and reception.
The forum is named for Joel Hardman, PhD, professor of Pharmacology, emeritus, who chaired the Department of Pharmacology from 1975 to 1990. For more information, contact Karen Gieg, Pharmacology education program manager, at 322-1182 or karen.gieg@vanderbilt.edu.
Photo: Pharmacology Forum
Pharmacology forum set for March 18
Pharmacology forum to explore neurobiology of criminal behavior
Reporter Department of Pharmacology Herbert Slatery III Joel Hardman neonatal abstinence syndrome opioid crisis Pharmacology Forum pharmacology lecture Reporter June 15 2018 Stephen Patrick


Annual or biannual wellness exams are the foundation of preventative care. These exams involve a thorough history including information about a pet's breed, age, lifestyle, behavior, and diet, followed by a comprehensive physical exam by your veterinarian who will then make recommendations for diet, blood work, vaccinations, diagnostics, or procedures based on their findings and your concerns. Medicine isn't one-size fits all and we evaluate all pets as individuals.
There is nothing in the world more exciting than bringing home your future best friend. We recommend that your new family member is seen by their veterinarian within the first week of coming home to ensure that they are healthy, doing well at home and to begin their personalized immunization schedule. Puppies and kittens are the most at risk group for infectious diseases.
Over the course of the puppy and kitten visits, we will discuss diet, spay/neuter, training, behavioral issues, and breed specific concerns.
The goal of the annual or biannual wellness exams is to monitor your pet's progress, catch diseases or illnesses early, and to update their immunizations, when appropriate. We start with a discussion of your pet's previously diagnosed illnesses, current medications, perceived comfort level, and any specific concerns that your might have and then move on to a thorough physical exam. Vaccine and screening recommendations are based on your pet's risks and your lifestyle. We generally recommend annual screening for infectious diseases such as lyme and heartworm disease, as well as intestinal parasites.
It is important to remember that for every year that passes, our pets age the equivalent of 5-8 years depending on their species and breed. The term "senior" literally just refers to age (>65yr human equivalent). Senior doesn't imply that they have age related diseases, but we are more likely to find certain disease in senior pets so additional screening tests are often recommended and we highly recommended wellness exams every 6 months.


Adarsha Gram Project-II, a project established and co-funded by the Ministry of Land, Government of Bangladesh and European Union . It is an important contribution to the Govt. of Bangladesh's poverty alleviation program. The objectives are to focus the extreme poor, homeless and provide them with a shelter or home and community infrastructure. Access to useful skills, practical knowledge and opportunity for their capacity building is also provided to enable and enhance their self-sufficiency.
Washing their hands before eating meals.
Take decision in the community level meeting.
Sufficient food, clothes and medicine for themselves.
Sending their children to regularly schools.
Read and write (most of the adult).
Now own houses and land.
Capable of continuing group activities.
Capable of continuing group capacities.