text:
Curbside Capsule: 1983 Dodge 600 – E-Class With Less Class
– Posted on August 21, 2021
(first posted 8/21/2015) In the Chrysler Corporation's lengthy history of badge engineering, a tradition that appears to be drawing to an end, usually you could count on the clone bearing the Chrysler nameplate to be the fussier-looking variant. Particularly during the 1980s, "Chrysler" often meant wire wheel covers, a vinyl roof, perhaps an upright grille and a smattering of chrome. The 1983 Dodge 600 bucked the trend by looking messier than its Chrysler E-Class counterpart, but the 600 endured while the E-Class was quietly discontinued after just two years.
Both the E-Class and 600 eschewed traditional Mopar nameplates for blatantly European ones. While the E-Class favored plush luxury, albeit not quite as plush as the related New Yorker, the 600 wore two hats: conventional family sedan and quasi-sport sedan. Plymouth missed out initially on a version of this E-Body relative of the K-Car, except in Canada where the Plymouth Caravelle debuted in 1983.
The range-topping 600 ES was Dodge's attempt at a cut-price Euro-fighter, a Mopar alternative to the Pontiac 6000STE offering uprated suspension and instrumentation as well as bucket seats and a console. You could option it with a baulky five-speed manual transmission, although initially the only engine was the same 2.2 four featured in the Aries. Journalists compared it to the 6000 and various European and Japanese rivals and found it lacking in both mechanical refinement and build quality but it was not entirely without charm, boasting competent handling and steering. It still lived in the shadow of the critical darling 6000 STE. Sales of the ES generally accounted for 30-50% of the 600's already mediocre volumes.
Those seeking more performance would have been pleased to find a turbo join the 600 range for 1984, and it was available in either plain, six-seater base trim or in the fancier ES.
With the arrival of the Lancer hatchback, the 600 was revised and repositioned. It lost the Mirada-inspired grille and fender vents, and adopted simpler lighting assemblies. Effectively, it was a Plymouth Caravelle with a crosshair grille. The European-style ES was dropped, leaving a choice of base or SE sedans. You could still get a turbo four, but the 600 was now plain old family transport.
Never a strong seller, the 600's sales volumes dwindled over its 1983-88 run despite the even older Aries selling strong right up until its demise in 1989. For much of the 1980s, Dodge simply lacked a strong-selling mid-size sedan. The Lancer experienced an even harder fall from grace.
By 1988, Dodge had launched the even more conservative Dynasty with an upright roofline and an available V6. Finally, for 1989 the boxy Spirit arrived and the 600 was gone. Despite the Taurus' revolutionary styling indicating a change in consumer tastes, the dowdy Dynasty and Spirit sold considerably better than their forebears. The 600 would become one of the forgotten Mopars of the 1980s.
Car & Driver's July 1983 "Escape from Baja" comparison test, one of my favorite comparison tests, which pitted the Dodge 600ES against the Pontiac 6000 STE, Audi 5000S, Datsun Maxima, VW Quantum, Saab 900 Turbo, Volvo 760GLE and Toyota Cressida
← Curbside Classic: 1985-89 Chrysler LeBaron GTS – Hatchback Setbacks
COAL: 2006 PT Cruiser Limited Edition – Late to the Party →
Posted August 21, 2015 at 6:28 AM
It looks like Iacocca and Co. were flaunting their Ford influence on these: The Fairmont-cribbed roofline, the Mark V vents cut in the side, the ads shamelessly comparing the car to a Mercedes…
I've never totally understood why the Dodge 600 (and its E Class/Caravelle twins) sold poorly and is so difficult to find today. Was it that they didn't offer enough improvements over the Aries/Reliant to justify their existence? Or was it that their "European" names had zero equity or memorability, and people forgot that these cars existed because there was nothing to call them? Sounds like Acura in a nutshell…
Posted August 21, 2015 at 11:20 PM
It wasn't just the 600 that sold poorly, relative to its Chrysler and Plymouth K-car twins. The Aries and 400 seemed to come up far short of the other division's K-car sales, as well. I get the feeling that consumers were either going to buy the cheapest possible K-car they could get (which meant a Reliant) or they were going to go the opposite end, and get the most loaded K-car possible, which would be one of the disguised Chryslers. IOW, the Dodge K-cars were neither fancy, nor cheap enough, to sell.
Or maybe it was just that no one really believed any of the sporty hype that Chrysler marketing was putting forth for a Dodge K-car. A cheapo Plymouth or tarted-up Chrysler were much easier to promote.
I like your link to the Car and Driver test. Read it a while back, and if I recall, didn't they Pontiac 6000 die and they just left it on the side of the road in Mexico?
MarcKyle64
That was back when C/D was fun to read. Now? Not so much.
No, it was the Maxima that died. They drove it through several feet of water and fried the PCM. They also damaged the 600ES.
Phil b
I really don`t have too much to say about these cars, but it is good to see snippets of Brooklyn, NY in the photos.
The most LOLworthy aspect of this car is the 600 SE nameplate on the trunk lid in the exact underlined font used by Mercedes
fintail jim
Would that Mercedes-Benz sold a 600 SE. Oh wait, There was the 300 SEL 6.3. I drove one once that belonged to a friend. The car was 35 years old but impressed the he!! out me. Then again it cost almost the same as two Cadillacs when new.
Poor American manufacturers: When they did decide to follow the European paradigm they got the size right and packaging, to a certain extent, but they really dropped the ball in terms of performance and quality – two things the Big Three was renown for just a decade or two earlier.
Frank Bray
These cars really should have sold better. In many ways, they were what the original K-cars should have been; a little bit longer, less boxy looking and with smoother styling. I particularly like the post-1984 models that took on the Caravelle look. Pitching these against the 6000STE as a performance model was a mistake with that wheezing 2.2 4-banger.
Which still leaves the question: what was it about these cars that the buying public just didn't like?
Maybe we need to look at the competition, since that's obviously what buyers did. 🙂
I think there was more than a little braggadocio going on with Lee and Chrysler at the time. And maybe a little butt hurt (after being fired from Ford) as the kids say now, too. We have a saying in the States, "Go big or go home", this may have been Lido's "go big…" moment.
I was never a fan of the blatant copying of Mercedes motifs back then, I thought the cars were as well engineered (but not necessarily assembled) as any other FWD cars of the time. When I came up with the term "Cockroach of the Road" for the GM X-bodies, it was because they were first. Had the K cars launched first, they could have been the archtypical CoTR instead. Except, they actually held up better (in most cases) than the X cars, doing their jobs until the level of neglect dictated their date with the crusher.
Another of the advertising themes during this time was "The competition is good, so we had to be better". Again, the cars may have been marginally better, but that kind of American "know how" and "can do" appealed (still appeals) to a certain demographic over here. I really believe it helped to sell cars to these people.
One more thought: Unlike today, where we have the same sausage, different lengths philosophy of car making/selling, I think Lido & Co., were trying anything/everything to get people to come into the showroom. Using the metaphor of a pizza parlor, who would go to one that only sold four sizes only of a pepperoni pizza? When I look back now, the amount of body styles and configurations coming out of Chrysler in the 1980's was really quite impressive, especially for a company that had been on the ropes a few years before.
In the end, they did garner some new buyers (I was one of them), but quality glitches and the fact that they were recycling the K car repeatedly put people off. Even the AA cars (1989+ Spirit and LeBaron), while probably the pinnacle of K development (WRT to durability) sold OK, but folks were ready for bigger, flashier cars. Chrysler couldn't do that with the K's, but the LHs were waiting in the wings.
On these and the convertibles i find the Mirada-inspired front clip strangely attractive. Supposedly there was acoupe…never seen one though.
Recently i came across a gold '85 turbo ragtop. A 3 owner car it was in great shape. The blackout trim and 'pizza wheels' meant that it in no way said 'chick car' despite being a small droptop. I wanted it as a summer cruiser to flip in a year or so. But his firmness on price 'sentimental value' left no meat on the bone…
The coupe was originally called the 400 and was a twin to the K-car Chrysler LeBaron (or looked at another way, a fancier Dodge Aries). I did see a few of these back in the day, but buyers far preferred a Chrysler badge, much as they did earlier with the Cordoba over the less prestigious Dodge Charger/Magnum/Mirada alternatives. Later coupes were badged 600 rather than 400 because, well, it must be worth more if the number is higher. It was still a non-stretched K-car without the sedan's extended wheelbase or higher trunk lid.
I may be in the minority, but I prefer the styling of the 600 to the Chrysler E-Class. While arguably busy, the Mirada inspired front was distinct and clearly conveyed Dodge's "face" to the world. The E-Class, with its LeBaron nose, looked exactly like the cars positioned above it (New Yorker) and below it in the line-up.
As others have noted here, I don't think the names on these cars did them any favors either. The names were utterly forgettable, and the cars were far from European, so it was probably hard to get people excited over them, versus just going for the understandable, basic transportation offered by the Aries/Reliant.
CJinSD
The 600 shared its nose with the 400, which was Dodge's short-wheelbase Lebaron K-car twin. The problem with the Dodge's nose is that they just didn't have the assembly precision or quality of materials to pull off the horizontal bars. They looked misaligned or damaged when they arrived in dealerships.
I actually remember hating this car when I was a pre-teen and noticing cars on the street.
Something about that c pillar kick.
The K-Car and K-Car based offshoots were nothing more but boring generic cookie cutter cars that I would never even considered even if one is given to me for free. Between these, the Pontiac A6000 (Dodge 600's chief competitor) and the Mercury Sable, I would rather get the Mercury Sable.
I would too, but remember the Sable arrived a few years after the 600.
I had a friend who was a Chrysler/Plymouth salesman at the time, and I remember him telling me how impossible it was to sell a Plymouth Caravelle after the Taurus dropped. Customers would look at this antiquated-looking thing in his showroom, laugh, and just walk away.
I've never found this vehicle very attractive. Its body is attractive, but the front end is hideous!
orangechallenger
Some pristine Dodge 600s are still seen in Michigan running around with municipal plates, in 2015.
principaldan
Lee Iaccoca was willing to try just about anything to get people to forget the "Bad Old Days" of the 1970s Chrysler Corporation wasn't he?
Could you get the SE with turbo AND 5 speed manual? That would be interesting but only if it had an aftermarket transmission parts fitted to improve the throws and shift quality.
Only in 1984 could you get the 5-speed and the 2.2 turbo. Once they switched to the luxury themed SE in '85, it was automatic only.
Had a Reliant wagon with the 5-speed, it was indeed baulky. There is no "feel" whatsoever, it's like the shifter isn't even connected to anything. That ad claiming driving superiority over the Benz is hilarious too. They didn't understand that bullshit ads like that actually hurt what little credibility they might have had? And spoken in such an authoritative and confident tone, too
Also they were comparing it to a 300D. The non-turbo W123 diesels were *notoriously* slow and far, far from a sports sedan. So saying that your "sports sedan" can offer a better driving experience than, essentially, a diesel taxi (though a very well assembled and appointed one) isn't exactly a herculean achievement!
Sports is about cornering the ability to carry speed through tight turns, 0-60 is superfluous if you have no reason to slow for turns.
Johannes Dutch
Plus the fact that a 0-60 sprint must have been highly illegal in the days that the national speed limit was 55.
suzulight
"Advanced front wheel drive performance" Now there's an oxymoron…
Howard Kerr
Apparently you've never driven an Acura Integra GS-R or RSX or any Audi product.
I think the lack of sales for the 600 and the E-Class is attributable to lack of a V6 and as with the Lancer discussed earlier…too many products from these 2 brands clustered around 1 price point.
The 600 looks like a Ford LTD (the smaller one) but Ford wasn't foolish enough to try to sell that with a 4 cylinder.
Actually Ford did sell Fox LTDs with the 2.3 Lima.
I recall Dodge using FWD as a selling point for the Omni-based Charger 2.2, unlike the Camaro and Mustang that still used "old-technology rear wheel drive". How times have changed…..
But there was a widespread perception in the early '80s that FWD was modern and RWD was becoming obsolete. Certainly, if your car had FWD at the time you promoted that fact (sometimes on a little plaque on the car itself), and if it was RWD you just didn't mention the drivetrain.
You need a five minute in town sprint in a Peugeot you'd never bother with RWD again.
Count me among those who like the Mirada-inspired nose better than the equivalent E-class, though I could have done without the fender vents. As I've mentioned before, I actually quite like the proportions of these cars. I've never driven one, and have only ridden in one of the convertibles, so I can't say a lot there. But in the looks department, they work for me. Seems much more appealing than the stubby 400 or the staid Aries, or even the overly severe Dynasty/
Chryslers badge engineering makes Rootes Group look like absolute amateurs or is that where they got the idea its certainly the same business plan, take one reasonably well made car and trim it in a multitude of ways to fit every pocket with slight powertrain variations to suit.
Rob Finfrock
If I ever bought one of these (I can't foresee that ever happening, but ya never know) the first thing I'd do is file down the drip rails to end at the rear quarter window. Crude 'shop:
Second quick PhotoShop. The extended drip rail (likely concealing the roof join line) always bugged me on these.
Isn't it ironic how the Chrysler version of this car was named E-Class way before Damiler had any interest in Chrysler. The name E-Class didn't work for Chrysler, but it surely works for Mercedes Benz !!!
I always thought the E-Class and the 600 looked way better then the New Yorker Turbo model with the formal vinyl roof cap, chrome roof band, and opera lamps. That model as just way over the top.
nrd515
A friend of mine who I've known for over 45 years now has had many bad bad cars. He's had some good ones, too, but most of the early ones were bad. And his '85 600 was the worst, nothing else comes close. It was blue, mid level trimmed, and I can't remember what engine it had, but it never went long without being behind a towtruck. A couple of times, it actually died within sight of the dealership right after spending a couple of days there getting "fixed". It was always electrical issues. After a couple of years of torturing him, it decided to strand him a mile from the dealership, and as he walked there, he decided, no matter what, it wasn't coming home with him. And it was gone. Traded that day for a Caravan, one of his best vehicles, no doubt. I always wondered what happened to the 600, and who was the poor bastard who bought it?
zwep
Posted September 6, 2021 at 12:35 PM
Funny thing, my Dad bought a new Dodge 600 in 1986, and it replaced the worst car he ever owned (a 1984 Pontiac Sunbird). The Sunbird was handed down to my youngest sister to take to college, after the engine had been replaced once (I think under warranty) despite dealer maintenance per schedule. It lost its timing belt with less than 1000 miles on it (new car basically) and had other problems like leaky power steering and crispy plastic switchgear which eventually broke. The replacement engine threw a rod, at less than 80k total miles, we junked it as a 5 year old car.
The 600 was OK, but my Dad didn't have it long before it was totalled in an accident my middle sister had when she borrowed it while her car was being worked on (coincidentally my Dad was in the hospital when that happened) after 3 years of ownership. Funny thing I remember about it that it was the first car in my family that had the high mounted stoplight and also 1986 was the last year you could claim interest from car payments on your federal tax deductions.
His was blue, too (light blue). Replaced with a 1989 Mercury Sable, first of 3 he was eventually to own (followed by 2 Impalas in a row, we still have the last one).
My brother in law had one of these back in the day, it looked exactly like the car in the first ad at the top of the post. I remember driving it (briefly) and being underwhelmed with the acceleration of the atmo 2.2. At the time, I had an Olds 442, so most anything new seemed rather weak…
I actually rather liked the car, it had all of the room of the contemporary FWD K bodies, but we (collectively) were still impressed with the amount of room you could get with the FWD layout. But I don't remember much more than that, as he only had the car a few years, as my nephews and niece were growing kids back then and a five passenger four door sedan wasn't going to work for very long.
It truly, truly was the definition of a shitty car.
Billinsavannah
My impression of Chrysler corp at that time was that they had a huge bin full of car parts. They would slap the parts together in a random fashion, drop in a 2.2, call it a new model then shamelessly advertise it as better than a Mercedes or BMW in some ridiculous category.
I had bought a new 1980 Dodge Omni 024 which was a pretty decent car but by 1982/83 when Chrysler's flogging of the K platform went into full swing, I was embarrassed to be driving a Dodge. Chrysler's advertising was blatantly false and insulted the intelligence of their potential customer. It turned me off and probably a lot of other people. Isuzu went the false advertising route with spokesman Joe Isuzu. With Isuzu, you knew they were jerking your chain and found it funny, and it sold cars.
Marky Mark
Good article! always liked these larger K-car sedans with the extra C-pillar windows. Here is a photo of the 1983-1985 Plymouth Caravelle sedan with its own unique grill.
Yep, put a horizontal slat grill on it, you got a Dodge, put a vertical slat grill, you got a Chrysler, put an egg rate grill, you got a Plymouth. I suppose if Desoto had been stil around in the 80s they would have slapped some sort of diagonal grill on it and called it an Adventurer.
Moparlee
I always found these cars just a fat looking K-car. I never saw these as a threat to Pontiac in any way. Or Chevy either (Lumina or Celebrity, not sure which was the market competitor).
Thomas Merjanian
Piece of garbage. We rented a 1983 600 six-passenger two-door in Los Angeles. On an expressway north of San Diego, our youngest child needed to go. So, first I opened the driver's door to exit and then open the passenger door to retrieve him. The door to my side was hardly opened when a tractor-trailer whizzed by in the right lane. The airflow around the rig wrenched the door FORWARD and displaced it from its hinges.
The two things I recall about the 600 were the appropriation of the Mercedes font for the model designation, complete with chrome bar underneath it, and the voice warning system for various maladies or reminders. Unlike the better-remembered system Nissan used at the time, Chrysler went with a male voice warning you a door was a jar. In any case, this car badly needed a smooth 6 cylinder engine to compete against the Taurus or even the GM A bodies.
VanillaDude
When I think of Dodge, I do not think of the 600 or anything like that. When you told someone one got a Dodge, they would imagine a sporty car – not a 600. Dodge is where you went for cheap sporty cars, not cheap luxury cars.
Throughout the 1970s we see Dodge attempting to hawk a personal luxury car – Charger SE, Magnum, Mirada, all unsuccessfully. The full size cars were also ignored – Monaco, Polara, Royal Monaco, St. Regis. If you wanted luxury from Chrysler – you got a Chrysler. If you wanted cheap – you got a Plymouth. If you wanted sporty – you got a Dodge.
Yet Dodge insisted in trying to sell luxury. Throughout the 1980s and 1990s, we see Dodge offering luxury versions of their cars without success. No one went to Pontiac for luxury, and no one went to Dodge either.
When did Dodge ever offer a successful luxury car? The best it did was during the 1960s with the Monaco, but even the Monaco didn't survive and was a perennial also-ran to Caprice, LTD, Bonneville and only outsold Ambassador DLO.
just sayin' Ma... on Vintage Ad: 1959 Daihatsu Trimobile – I Had No Idea These Were Sold Here
justy baum on COAL Capsule: So…This Is What Filming A Movie Is Like?
Carey Frisch on Curbside Classic: 1977-79 Mercury Cougar XR7 – The First Thundercat


Every homeowner will feel comfortable if the bathroom is clean and neat. By doing some remodeling, the homeowner can make the bathroom look better. There are many designs, style, and furniture for the bathroom. Due to that situation, the homeowner must make the bathroom remodel checklist to focus on remodeling, buying, designing the bathroom which is suitable. The homeowner must make sure that the style is appropriate because it makes the content of the style costs properly. Here are some checklists that the homeowner must do before remodeling the bathroom.
The budget is one of the important points that You should not forget when you make your bathroom remodel checklist. If the homeowner has designed the style and the theme of the bathroom, the homeowner must calculate how much the budget to spend on remodeling the bathroom. Setting the budget helps and guides the homeowner to make a decision about what should be bought to remodel the bathroom. Once, the home owner knows about the amount which is allocated to choose the tiles, paint, shower, faucet, etc. the budget is including paying the workers. Some people think about the limit cost in hiring workers to renovate the bathroom. But on the other hand, hiring a worker to make the bathroom makes the desirable result. It's a smart idea to hire worker because the remodeling bathroom is quite complex and a difficult job. Therefore, hire workers can save the time and burden in remodeling the bathroom.
Remodeling the bathroom isn't completed without rearranging the furniture or repair the furniture such as shower, bathtub, toilet, sink, faucet and the shower head. Besides, the homeowner must concern and update about the glass door or the paint whether the homeowner wants to use paint or wallpaper. The homeowner can change the look of the bathroom by changing the drawer pulls, the door handle, the cabinet, and so on. The cabinet and the storage racks are also necessary. In the small bathroom, the homeowner must concern about the simple and small furniture either. The stuff must be fit and both style and size for the bathroom. All the needs you have to input into Your Bathroom Remodel Checklist. However, this must also be tailored to your needs and also your budget.
A bathroom must have adequate lighting for the convenient and the security aspects. Remodeling bathroom with the natural light bathroom space and add lamps inside the bathroom.
Ventilation is very important especially for a wet area like a bathroom. It's also a complex task that requires proper planning such as choosing the good fan, the right position for the door or other installing, and installing of the electrical wire.
That's some important points to become the reference when you make your bathroom remodel checklist. Proper planning when you are going to do, the bathroom renovation project can generate appropriate bathroom of your dreams.


text:
\section{Introduction}

The distribution of neutral hydrogen (HI) in the Universe contains a wealth of cosmological information.
During the dark ages, the HI fluctuations follow the dark matter  density perturbations;
while during the epoch of reionization (EoR),
the HI is anti-correlated with ionizing sources,
and deviates from the total matter distribution.
After reionization, however, most HI resides in halos, and once again can be used as
a tracer of the large scale structure (LSS) of matter distribution over a wide range of redshifts and
scales \citep{Wang2019}. Indeed, the 21 cm intensity mapping technique has been developed to more efficiently map the
LSS of the Universe using HI as the tracer \citep{Peterson2009}.
This technique is a promising probe of cosmological models (\citealt{Bull2018,Xu2015A,Xu2016A,Obuljen2018b}).

The 21 cm signals from the neutral component of the IGM are almost the unique feasible probe to major epochs of reionization by using current or
upcoming radio telescopes \citep{Alvarez:2019pss,Furlanetto:2019jzo,Liu:2019srd}, such as the PAPER \citep{Parsons2010}, MWA
(\citealt{Bowman2013,Tingay2013}), LOFAR \citep{vanHaarlem2013}, HERA \citep{DeBoer2017}, SKA \citep{Koopmans2015}.
However, reionization is a complicated process and at present our understanding is still mostly speculative.
As other tracers of large scale structure, it is generally believed that on large scales the density of the
neutral hydrogen should be proportional to the dark matter (DM) density with a nearly constant coefficient which we shall call ``bias''.
In order to interpret the upcoming 21 cm data from the EoR experiments, it is imperative to know the evolution and
the scale-dependence of the bias of HI distribution, as well as the physical basis of its behavior.

There have been a number of investigations for the HI bias in the local and post-reionization Universe,
using both observations and theory. For the low-redshift Universe,
\citet{Martin2012} analyzed the bias of the HI-selected
galaxies with $z \lesssim 0.06$ in the ALFALFA survey, and found that on scales
$\lesssim 10$ $h^{-1}$Mpc, the HI-selected galaxies are anti-biased with respect to DM, while on
scales $\gtrsim 10$  $h^{-1}$Mpc they are roughly unbiased. This is consistent with an earlier
analysis for HIPASS samples \citep{Basilakos2007}. \citet{Marn2010} developed an
analytic framework for the large-scale HI bias based on dark matter halo
bias and a HI mass-halo mass relation. In \citet{Bagla2010} and \citet{Sarkar2016},  the HI power spectrum
and the related HI bias are derived by populating HI in halos identified in DM-only simulations.
The HI bias in a wide redshift range ($0<z<5$) was investigated more explicitly by hydrodynamic
simulations in \citet{Navarro2018}.  To model the multi-phase hydrogen, they also post-processed
the star-forming gas. They found that even at $z\sim3$, the HI bias is
already non-linear at $k\gtrsim 0.3~h$Mpc$^{-1}$.

During the EoR, however, most of the HI resides in the IGM.
Various processes such as the formation of early galaxies and the non-linear bubble growth
significantly complicate the bias of the HI distribution from the DM distribution.
HI is not a very good tracer of the DM during this epoch, but it encodes rich
information of reionization process and its driving sources. \citet{Hoffmann2018} have
developed a quadratic model for the HI bias, which was found
to work well during the early stage of reionization, and suggested that measurements of the
three-point correlation functions in observations can constrain the astrophysical processes
driving the reionization. \citet{McQuinn2018} developed an effective perturbation theory,
in which the 21 cm bias is expanded as the sum of terms whose
coefficients reflect the bias of the ionizing sources, the global neutral fraction, the
characteristic size of ionized regions and the patchiness of reionization. Still, the HI bias
during the EoR is much less studied, especially for the transition stage:
from the late EoR to the post-reionization. During this stage, the HI distribution is
dominated by both the remaining neutral gas in halos, and the relic voids yet to be ionized,
i.e., the ``neutral islands'' \citep{Xu2014,Xu2017}. The HI bias may show complicated and
interesting behaviors. Knowing the HI bias would be convenient  for deriving HI distribution
statistics from the more simple dark matter distribution in theoretical works. In this work we shall study
the HI bias during the EoR, especially in the transition era.

This paper is organized as follows. In Section ~\ref{sec:model}, we present a model
for the HI distribution during the EoR, including both the HI in the IGM from a set of semi-numerical
simulations, and the HI in halos based on an empirical model.
The results of the evolution and the scale dependence of the HI bias and 21cm bias are presented in
Section ~\ref{sec:results}. We summarize and discuss our results in Section ~\ref{sec:conclusions}.
Throughout this paper, we assume the $\Lambda$CDM model and adopt the
following cosmological parameters :
$\Omega_{\rm b} = 0.045$, $\Omega_{\rm m} = 0.27$, $\Omega_{\Lambda} = 0.73$,
$h = 0.7$, $\sigma_8 = 0.8$, and $n_{\rm s} = 0.96$.

\section{The HI Model}
\label{sec:model}

During and before the EoR,  the neutral hydrogen exists in both IGM (as large diffuse patches of gas) and halos (as small dense clumps).
We shall include both components in our model to properly account for the HI distribution.

\subsection{The HI in the IGM}

\begin{figure*}
\centering
\subfigure[z=9.0,\ $\bar{x}^{\rm IGM}_{\rm HI}$=0.82]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=3.8in]{fig_z9000.png}
\end{minipage}%
}%
\subfigure[z=7.8,\ $\bar{x}^{\rm IGM}_{\rm HI}$=0.53]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=3.8in]{fig_z7875.png}
\end{minipage}%
}\\
\subfigure[z=6.7, \ $\bar{x}^{\rm IGM}_{\rm HI}$=0.14]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=3.8in]{fig_z6700.png}
\end{minipage}%
}%
\subfigure[z=6.5,\ $\bar{x}^{\rm IGM}_{\rm HI}$=0.025]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=3.8in]{fig_z6500.png}
\end{minipage}
}%
\centering
\caption{A visualization of the evolution of the ionized field of the simulation (1Gpc). The mean neutral fractions for the four panels are
 0.82, 0.53, 0.14 and 0.025 respectively.
}
\label{fig:field}
\end{figure*}

It is generally believed that reionization started first in high density regions where the first luminous objects formed first.
In the ``bubble model''  of reionization \citep{Furlanetto2004}, the amount of star formation and the resulting ionizing photons are
estimated using the excursion set model. Based on this idea, the so called ``semi-numerical simulations" have been developed.
For example,  \citet{Mesinger2011} developed the {\tt 21cmFAST}\footnote{https://github.com/andreimesinger/21cmFAST}, to
simulate the evolution of the 3D density, ionization and 21cm brightness temperature fields efficiently.
The ``bubble model'' considers spherical regions of increasingly smaller scales
and identifies ionized bubbles by comparing the cumulative number of ionizing photons
produced within the region with the number consumed in reionization process.
It has been demonstrated that the statistical predictions of the ``bubble model'' and the {\tt 21cmFAST}
agree fairly well with radiative-hydrodynamic simulations \citep{Zahn2007,Mesinger2011,Zahn2011}, at least when recombination,
feedback, etc. are ignored. However, during most epochs of reionization, the topology of the ionization field is much more complicated than
the isolated bubbles configuration. The bubbles start to connect with each other as early as
when the global ionized fraction is just about 10\%, and the Universe starts the percolation
process when the ionized fraction gets $\sim$ 30\% (see e.g. \citealt{Furlanetto2016,Chen:2018enj}).
Inspired by the bubble model, the {\tt 21cmFAST} determines the ionization state of each point by comparing the expected
ionizing photon production in the surrounding region with the required number, but it allows non-spherical geometry for the ionized regions.
In order to give a better description of the evolution of neutral regions after percolation,
\citet{Xu2014} developed the so-called ``island model'', assuming isolated  neutral islands topology.
The island model also takes into account an ionizing background that is inevitable during the late EoR
\citep{Furlanetto2005,Emberson2013,McQuinn2011}.
Based on the ``island model'', a semi-numerical code named {\tt islandFAST} was developed to mimic
the islands evolution during the last stage of reionization \citep{Xu2017}.
In the {\tt islandFAST}, the effect of small-scale absorbers is taken into account empirically by adopting
a fitting formula for the evolution of mean free path (MFP) of ionizing photons \citep{2010ApJ...721.1448S}, based on the
observed number density of Lyman limit systems up to redshift 6. Before the completion of reionization, the MFP is limited
by both the under-dense islands and the over-dense absorbers. The evolution of the ionization field and the intensity of the
ionizing background are derived self-consistently by an iterative procedure to ensure convergence in the total effective
MFP of the ionizing photons.

Topological analysis shows that the islands become mostly isolated when the global neutral
fraction reduces to $\bar{x}_{\rm HI}\sim 0.16$ in a model with parameters similar to the present case \citep{Chen:2018enj}.
In the island model the early stage of reionization is identical to that of
the bubble model ({\tt 21cmFAST}) until $\bar{x}_{\rm HI} \approx 0.17$, slightly before the isolation of individual islands, after
which the island model criterion is applied for the later stages of reionization.
For the following analysis, our simulation has a box size of 1 Gpc (comoving) on a side and
a resolution of $500^3$ cells. An ionizing efficiency parameter of $\zeta = 20$ and a minimum
virial temperature of $10^4$ K are adopted for host halos of ionizing sources.
A few slices of the ionization field at several snapshots are shown in Fig.~\ref{fig:field} .

\subsection{The HI in halos}
\label{sec:massfunction}
To model the HI in halos, for each cell in the simulation box with a size of $V$ and a mass of $M$ at redshift $z_0$,
the number density of halos with mass $m$ virialized at $z_{1}$ in this cell, $n(m,z_{1}|M,V,z_{0})$,
can be estimated by using the conditional mass function \citep{Cooray2002}:
\begin{eqnarray}
    \frac{m^{2}n(m,z_{1}|M,V,z_{0})}{\bar{\rho}_m}\frac{dm}{m} &=& \nu_{10}f(\nu_{10})\frac{d\nu_{10}}{\nu_{10}},
	\label{eq:conditional}
\end{eqnarray}
where
\begin{eqnarray}
    \nu_{10} &=& \frac{[\delta_{\rm sc}(z_{1})-\delta_{0}(\delta, z_{0})]^{2}}{\sigma^{2}(m)-\sigma^{2}(M)}.
	\label{eq:nu}
\end{eqnarray}
Here $\bar{\rho}_m=\rho_c\Omega_m$ is the mean matter density of the present Universe and $\rho_c=3H^2_0/8\pi G$ is the critical density; $\delta_{\rm sc}(z_{1})$ is critical density required for spherical collapse at $z_{1}$,
$\delta_{0}(\delta, z_{0})$ denotes the initial density for a region to have density $\delta$ at $z_{0}$,
$\sigma^{2}(m)$ is the variance of the density fluctuations on scale $m$,
and we adopt the form of $f(\nu)$ given in \citet{Sheth1999}.
The relation between the HI mass and its host halo mass has been widely
studied \citep{Gong2011, Popping2015,Guo2017,Padmanabhan2017,Navarro2018,Obuljen2018a}.
Here we adopt the results from a large state-of-the-art hydrodynamic simulation,
 TNG100 \citep{Navarro2018}, for which the result can be fitted by
\begin{eqnarray}
    m_{\rm HI}(m, z) &=& m_{0}\left(\frac{m}{m_{\rm min}}\right)^{\alpha}\exp\left({-\frac{m_{\rm min}}{m}}\right).
	\label{eq:himass}
\end{eqnarray}
The parameters are given for a number of redshifts. At $z\sim5$, $m_{\rm 0} = 9.5 \times 10^{7} h^{\rm -1}M_{\odot}$,
$m_{\rm min} = 1.9 \times 10^{9} h^{\rm -1}M_{\odot}$, and $\alpha = 0.9$ \citep{Navarro2018}.
We adopt these $z\sim5$ parameter values throughout the reionization history, as that is the highest redshift where the
values are given, and also the relations vary little near $z\sim5$. Another possibility is to fit the redshift dependence
at $z\lesssim5$, then extrapolate to higher redshifts. We have checked that such extrapolation gives similar results,
but given the uncertainty,  it is not clear if a better accuracy can be achieved.
The HI content of a halo may also depends on its assembly history and when the local patch was ionized.
Obviously, there are always some theoretical
uncertainties in the model of HI gas in halos during the EoR,
both intrinsic and environmental, which one must bear in mind.

The neutral fraction of a given cell with mass $M$ and volume $V$ contributed by HI in halos can be written as
\begin{equation}
    x^{\rm halo}_{\rm HI} (M,V,z) = \frac{1}{\rho_c\Omega_{\rm b}X_{\rm H}}\int_0^\infty n(m,z|M,V,z)
    m_{\rm HI}(m, z)\, {\rm d}m,
	\label{eq:rho}
\end{equation}
where $X_{\rm H}$ donates the hydrogen mass fraction in the gas, $X_{\rm H} \sim 0.75$.
The HI in halos are combined with the HI in the IGM, predicted by semi-numerical simulations such as
 the {\tt 21cmFAST} or {\tt islandFAST}, to generate
the full HI field at various redshifts throughout the reionization.
In the following, we denote the neutral fraction in the IGM as $x^{\rm IGM}_{\rm HI}$,
the neutral fraction contributed from the HI in halos as $x^{\rm halo}_{\rm HI}$, and denote
the total neutral fraction as $f_{\rm HI}$.

\section{The HI Bias throughout the EoR}
\label{sec:results}

The formation of galaxies and the evolution of the IGM are physical
consequences of the primordial density perturbations. On large scales,  the observables such as
the galaxy number density, the neutral hydrogen fraction of the IGM or the 21cm brightness temperature should be related to the
locally averaged matter density. Here we approximate such relation with a linear model,
 though more generally the relation may be non-linear and stochastic \citep{1999ApJ...520...24D}.

The reionization process is believed to be ``inside-out'' (e.g. \citealt{Iliev2006,Trac2007})
on large scales: galaxies formed firstly in over-dense regions, and ionized their surrounding gas,
then the reionization proceeds from the over-dense regions to the mean and under-dense regions.
In this scenario, it is expected that the neutral hydrogen is anti-correlated with the underlying dark matter
density distribution on large scales. However, this relation could be inverted on small scales, where the
neutral hydrogen in halos is correlated with the density, and also the ionization front moves faster into the void regions.
The non-linear structure growth, galaxy formation, ionizations and feedbacks would significantly
complicate the neutral hydrogen-density relation and hence the HI bias. The time- and scale-dependence
of the HI bias encodes rich information about the reionization process.

The neutral hydrogen is observationally traced by the 21 cm signal, the
upcoming low-frequency interferometers will directly measure the fluctuations in the 21 cm brightness temperature.
Ignoring the peculiar velocities, the 21 cm brightness temperature is related to
the neutral fraction $f_{\rm HI}$, the density contrast $\delta$, and the spin temperature $T_{\rm s}$
via (e.g. \citealt{Pritchard2012})
\begin{equation}
    \delta T_{\rm b} = 27\, f_{\rm HI}(1+\delta)\left(\frac{\Omega_{\rm b}h^{2}}{0.023}\right)
    \left(\frac{0.15}{\Omega_{\rm m}h^{2}} \frac{1+z}{10}\right)^{1/2}\left(\frac{T_{\rm s} - T_{\gamma}}{T_{\rm s}}\right)\, {\rm mK},
	\label{eq:21cmbrightness}
\end{equation}
where $T_{\gamma}$ is the background photon temperature, and in the absence of very strong radio sources it would be given by the
cosmic microwave background temperature at that redshift. Although when the first stars formed $T_{\rm s}$ might be lower than
$T_{\gamma}$ \citep{2004ApJ...602....1C,2008ApJ...684...18C},  after a moderate fraction of gas had been ionized, the rest of the neutral HI would
be heated to $T_{\rm s} \gg T_{\gamma}$. For simplicity here we shall assume this relation holds through the whole EoR process.
To calculate the contributions to the 21cm signal from halos and the IGM separately, one can replace the $f_{\rm HI}$ with $x_{\rm HI}^{\rm halo}$
or with $x_{\rm HI}^{\rm IGM}$. Strictly speaking, Eq. (\ref{eq:21cmbrightness}) is only valid in the optically-thin limit, which may not be true
for HI gas in halos. However, it has been shown that for the average of $\delta T_b$  from many halos, it is still
a good enough approximation \citep{Yue2009}.

  The neutral fraction bias can be computed by comparing the power spectra of
the neutral fraction field and dark matter density field, either from the auto-power spectrum
\begin{eqnarray}
    b^2_{f}(k) &\equiv& P_{\rm HI}(k)/P_{\rm \delta \delta}(k),
	\label{eq:bias1}
\end{eqnarray}
or from the cross-power spectrum
\begin{eqnarray}
    b_{f}(k) &\equiv& P_{\rm HI \delta}(k)/P_{\rm \delta \delta}(k);
	\label{eq:bias2}
\end{eqnarray}
where
\begin{eqnarray}
P_{\rm \delta \delta}(k)&=&\mean{\hat{\delta}_m(k) \hat{\delta}^*_m(k)}^\prime,\nonumber\\
P_{\rm HI}(k)&=&\mean{ \hat{f}_{\rm HI} (k) \hat{f}^*_{\rm HI} (k)}^\prime,\\
P_{\rm HI \delta}(k)&=&\mean{\hat{f}_{\rm HI}(k) \hat{\delta}^*_m(k)}^\prime\nonumber
\end{eqnarray}
 are the matter power spectrum, neural fraction power spectrum, and cross-power spectrum between the two,
 respectively,  $\hat{f}_{\rm HI}$ and $\hat{\delta}(k)$ are the Fourier transform of $f_{\rm HI}$ and dark matter density contrast respectively, and $\mean{}^\prime$ denotes the  the expectation value with the Dirac delta function removed.
  The bias defined in this way can be negative, this is similar to the bias of voids \citep{Sheth:2003py,Chan:2014qka}.
We shall use Eq. (\ref{eq:bias2}) which is less affected by the stochasticity and the shot noise term \citep{Navarro2018}, and also there is no
ambiguity in the sign of the bias.
Similarly, we also compute the 21cm bias using
\begin{eqnarray}
b_{21}(k)&\equiv& P_{T\delta}(k)/P_{\delta\delta}(k),
\label{eq:bias3}
\end{eqnarray}
where $\hat{\delta}_T(k)$ is the Fourier transform of $(\delta T_b-\mean{\delta T_b})/\mean{\delta T_b}$ and
$P_{T\delta}(k)=\mean{\hat{\delta}_T(k) \delta^*_m(k)}$. Throughout this paper for the 21cm power spectrum or 21cm-dark matter
cross-power spectrum we adopt the dimensionless definition.

\subsection{The power spectra}\label{sec:ps}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{PS_HIHI.pdf}
\includegraphics[width=0.5\textwidth]{Ps_tt_sim_model.pdf}
\caption{The neutral fraction ({\it upper panel}) and the 21 cm
power spectra ({\it lower panel}) predicted by the {\tt islandFAST} (black lines) as compared with the one
predicted by \citet{BTCL2013} (green line, denoted by ``Trac-100'' in the legend) and
the ones from \citet{2016MNRAS.456.3011D} (magenta lines, denoted by ``Iliev-244'').
The mean neutral fraction of each line is indicated in the legend.}
\label{fig:island21cmps}
\end{figure}

\begin{figure}
\centering
\subfigure[Dark matter power spectrum]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=0.9\textwidth]{Ps_dd_1Gpc_allz_nf_v4.pdf}
\end{minipage}%
}
\subfigure[Neutral fraction power spectrum]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=0.9\textwidth]{Ps_ii_1Gpc_allz_nf_v4.pdf}
\end{minipage}%
}
\subfigure[21 cm power spectrum]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=0.9\textwidth]{Ps_tt_1Gpc_allz_deltat.pdf}
\end{minipage}%
}
\centering
\caption{The power spectra of dark matter ({\it top panel}),
the HI neutral fraction $f_{\rm HI}$ ({\it middle panel}),
and the 21 cm brightness temperature ({\it bottom panel}).
The three curves are taken at $z = 10.0$, 7.88 and 6.45, corresponding to IGM mean
neutral fraction $\bar{x}^{\rm IGM}_{\rm HI} = $0.92, 0.53, and 0.011 respectively.
}
\label{fig:ps1}
\end{figure}

In the present work, the reionization process is simulated by the {\tt 21cmFAST} for early stage and by
the {\tt islandFAST} after percolation.
The 21 cm power spectrum predicted by the {\tt 21cmFAST} was previously presented and discussed in
\citet{Mesinger2011}. While the 21 cm power spectrum during the late stages of reionization was also
discussed in \citet{2019arXiv190301294G},
here we compare the {\tt islandFAST} predictions with the radiative-hydrodynamic simulations by
\citet{BTCL2013} (Trac-100 simulation) and by \citet{2016MNRAS.456.3011D} (Iliev-244 simulation)
at some similar neutral fractions. The neutral fraction power spectra and the 21cm power spectra,
in the limit of $T_{\rm s} \gg T_{\gamma}$,
are plotted in  the upper and lower panels of Fig.~\ref{fig:island21cmps}, respectively.
The black solid and dashed lines
correspond to neutral fractions of $x_{\rm HI} \sim 0.01$ and 0.14, respectively
from {\tt islandFAST}.
Here the box sizes are $200~h^{-1} \ensuremath{\,{\rm Mpc}}$ for the
Trac-100 simulation (green line), and $244~h^{-1} \rm{Mpc}$ for the Iliev-244 simulation
(magenta lines), respectively.
Generally, these neutral fraction and the 21 cm power spectra have similar shape on large scales.
 Considering the differences between the two numerical
 simulations and output neutral fractions, these differences are probably not very significant, though
the inclusion of {\it evolutional} small scale ionizing photons absorbers in the {\tt islandFAST}
semi-numerical code may also contributed to the difference.

The dark matter density power spectra (e.g.\citealt{2010MNRAS.406.2421S,2014MNRAS.439..725I}),
as well as the 21 cm power spectra (e.g. \citealt{Mesinger2007,2016MNRAS.455.4498K}) during the EoR
have been studied in a number of previous simulations.
In this subsection, we calculate the power spectra from our simulation, in the same convention
as the ones in the bias formula (Eq.(\ref{eq:bias2}) -- (\ref{eq:bias3}) ).
In addition to the matter density and 21 cm power spectra, here we also calculate the
neutral fraction power spectra, as well as the cross-power between them,
in order to gain a better understanding of the bias behavior to be presented in the next subsections.

In Fig.~\ref{fig:ps1} we plot the dark matter power spectra (top panel), the power spectra for
the neutral fraction $f_{\rm HI}$ field (middle panel) and 21cm brightness temperature field (bottom
panel) in our model during the EoR. In the top panel, the three curves from bottom to top are for the early,
intermediate and late stages of reionization, respectively, and in the middle and bottom panels
the corresponding curves are plotted with the same colors as the top panel.

 The power spectrum of the dark matter density fluctuations
steadily increase as the redshift decreases, while keeping the shape almost unchanged on the scales
discussed here.  By contrast, neither the redshift evolution nor the scale dependence of  the
neutral fraction power spectrum is monotonic. The neutral fraction power spectrum first increases during the
early stage of reionization, and then decreases during the late stage of reionization. The
21cm power spectrum, however, keeps increasing with decreasing redshift until  $x_{\rm HI}^{\rm IGM}\sim0.01$.  Note here
we are referring to the dimensionless power, and part of the increase of the power comes from the decreasing  mean 21cm brightness temperature
as more regions are ionized. In the late stage of reionization, there is a bump around $k\sim 0.1~h$/Mpc
on both of them. This scale is close to the typical ionized bubble size, and the HI fluctuations at smaller scales
are somewhat suppressed by reionization process.

The cross-power spectrum between the neutral fraction field and the dark matter density field is shown in
Fig.\ref{fig:ps_HIpower}.
We use dashed lines to mark the negative power, while solid lines refer to positive power.
As seen in this figure, during most of the EoR stages, the neutral fraction field is anti-correlated
with the dark matter density field, resulting in negative cross-power spectrum.
As the reionization proceeds, the amplitude of the large scale cross-power spectrum increases during the early stage of
reionization, reaches its maximum roughly at the mid point of reionization, then decreases during the late stage.
When the IGM global neutral fraction drops below $\sim 5 \%$, on the small scales a positive cross-correlation appears.
At this stage, most of the IGM has been ionized, while the neutral hydrogen in halos starts to dominate the cross power spectrum,
producing the positive correlation seen in the small scale power spectrum.
As the remaining neutral islands in the IGM shrink and decrease in number, the halo HI  come to dominate the fluctuations on larger and
larger scales, as a result this positive-to-negative transition point on the cross-power spectrum moves to larger scales.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Ps_id_1Gpc_allz_nf_v4.pdf}
\caption{The cross-power spectrum between the neutral fraction and the dark matter density.
The solid and the dashed lines represent positive and negative values respectively.
}
\label{fig:ps_HIpower}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Ps_td_1Gpc_highz_deltat_total.pdf}
\includegraphics[width=0.5\textwidth]{Ps_td_1Gpc_lowz_deltat_total.pdf}
\caption{The 21 cm brightness temperature and the dark matter density cross power spectrum.
Top panel:  early EoR; Bottom panel:  late EoR. Solid and dashed lines represent positive and negative values respectively.
}
\label{fig:ps2}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Ps_tt_all_1Gpc_nodelta.pdf}
\centering
\caption{The 21cm power spectrum contributed from the HI in the IGM (dotted lines), the one from the HI in halos (dashed lines), and the total 21cm power spectrum (solid lines).}
\label{fig:antoPS}
\end{figure}

The cross-power spectrum between the 21cm brightness temperature and the dark matter density
are plotted in Fig.~\ref{fig:ps2}. We use the two panels to show the early and late stages of reionization respectively.
We find that at the very beginning of reionization, the 21cm-dark matter cross-power spectrum is positive on all scales,
implying that the neutral hydrogen density fluctuations still follow the dark matter density fluctuations, although some rare
density peaks have been ionized. As more and more IGM around density peaks becomes ionized, the 21cm-dark matter
cross-power spectrum decreases, and transits to negative starting from the largest scales.
Then the large scale 21cm-dark matter cross-power becomes more and more negative. The amplitude reaches its maximum
at around $x_{\rm HI}^{\rm IGM}\sim0.1$, and decreases again. Different from the $f_{\rm HI}$-dark matter cross-power, the 21cm-dark matter cross-power spectrum is always positive at small scales, indicating that when weighted with the local density, the small scale 21 cm signal is always dominated by the HI in halos.
At the very late stage of reionization, the positive-to-negative transition scale increases rapidly.

In this plot the 21cm-dark matter cross-power spectrum at $z=9.90$ shows some oscillations, which are likely statistical fluctuations.
To check this interpretation,  we estimate the errors on cross-power spectra by using the jackknife resampling method.
In Fig. 5 we plot the errors for the z=9.90 and z=9.00 curves.
 To avoid clutter, errors of other curves are not shown there. We see that indeed at z=9.90 the error bars are larger than the
 oscillation feature on  the power spectrum curve, so it is likely that these are just statistical fluctuations. We also check that at z=9.00 the errors are
comparable with the z=9.90. However, at z=9.00 the cross-power spectrum is much larger than z=9.90. In logarithmic axes apparently
 its errors are less obvious than z=9.90.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Ps_ih_1Gpc_highz_deltat.pdf}
\includegraphics[width=0.5\textwidth]{Ps_ih_1Gpc_lowz_deltat.pdf}
\caption{The cross-power spectrum of the 21cm brightness from the HI in the IGM and that in halos.
The top panel shows the cross-power spectrum during the early EoR, and the bottom panel shows the
results during the late EoR. The solid and the dashed line represent positive and negative values respectively.
}
\label{fig:crossPS3}
\end{figure}

We then turn to the individual contribution from the IGM and halos to the 21cm power spectrum, see  Fig.~\ref{fig:antoPS}.
The power spectrum of the HI in the IGM evolves markedly, in contrast to the power spectrum of the HI in halos.
During the era studied here, the full 21cm power spectrum is dominated by the IGM contribution in our model, though we note here
that we assumed a constant $m_{\rm HI}-m$ relation, if it evolves this conclusion would be revised, though the evolution in this relation
is perhaps still much less significant than that in the IGM.

Fig.~\ref{fig:crossPS3} shows the cross-power between the 21cm brightness contributed from the IGM and
that from halos during the early (top panel) and late EoR (bottom panel). Generally these two components are anti-correlated
during the EoR, except at the very early stage ($x_{\rm HI}^{\rm IGM} \gtrsim 0.94$) when the ionized bubbles only occupy a tiny
fraction, there are still positive cross-correlation on large scales ($k \lesssim 0.1$ $h${\rm Mpc}$^{-1}$).

\subsection{The neutral fraction bias $b_{f}$}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Bias_1Gpc_allz_v4.pdf}
\caption{The HI bias at various redshifts.
}
\label{fig:ps_HIbias}
\end{figure}

In Fig.~\ref{fig:ps_HIbias}, we show the scale dependence of the neutral fraction bias
at various stages of reionization.
As the dark matter power spectrum evolves almost self-similarly throughout the EoR, the evolution of
neutral fraction bias $b_{f}$ basically follows the trend in the cross-power spectrum $P_{\rm HI \delta}$.
As discussed above, during most of the EoR the HI in the IGM makes a negative contribution to the bias,
while HI in halos makes a positive contribution. Before the end of reionization, the total bias is negative
on large scales. When $x_{\rm HI}^{\rm IGM}\gtrsim0.08$, it is negative on all scales, which is
expected in the ``inside-out'' model of the reionization process. In over-dense regions,
the HI {\it fraction} is lower than in the under-dense regions, resulting in an anti-correlated
$f_{\rm HI}-\delta$ relation. Note however that the absolute amount of the remaining HI content
in the over-dense regions is not necessarily smaller than in the under-dense regions.
Regarding the $k$-dependence of the $b_f(k)$, there is a typical scale,  below which $b_f$ drops
gradually, while almost independent of $k$ above this typical scale.
This typical scale increases as reionization process goes on, reflecting the bubble growth process during the EoR.

We do expect the bias $b_f$ to be scale-independent on large scales: if we smooth the density field
by a filter much larger than ionized bubbles, the density field becomes rather smooth, i.e. $\bar{\delta} \ll 1$, where $\bar{\delta}$ is the mean density contrast within the smoothing radius.
 In such case for a region with mass $M$ and mean density contrast $\bar{\delta}$ the mean neutral fraction $x_{\rm HI}(\bar{\delta})\sim1-\zeta/(1+n_{\rm rec}) f_{\rm coll}(\bar{\delta})$, or $\Delta x_{\rm HI}(\bar{\delta})\propto -\Delta f_{\rm coll}(\bar{\delta})$, where
\begin{equation}
f_{\rm coll}(\bar{\delta},M,z)={\rm erfc}\left[ \frac{\delta_c(z)-\bar{\delta}}{ \sqrt{2(\sigma^2(M_{\rm min})-\sigma^2(M)) } } \right]
\end{equation}
is the collapse fraction and $n_{\rm rec}$ is the mean recombination number per H atom.
For $\bar{\delta} \ll 1$ we have $\Delta f_{\rm coll} \propto \bar{\delta}$,  and as a result at large scale the HI bias is broadly scale-independent.

When $x_{\rm HI}^{\rm IGM}\gtrsim0.08$, HI in the IGM is dominant and the halo HI has a negligible contribution to the total HI.
During this stage, on small scales the amplitude of the negative bias decreases rapidly as reionization proceeds. However, on
large scales, at the beginning the amplitude is smaller, because $f_{\rm HI}$ is rather uniform and close to
$\sim1$ almost everywhere. As $x_{\rm HI}^{\rm IGM}$ decreases , the $b_f$ amplitude first increases to a peak amplitude $\sim 3$
 when the Universe is about half-ionized, then decreases as well. When $x_{\rm HI}^{\rm IGM}$ decreases to
 below $\sim0.08$, HI in halos starts to dominate the small scale $f_{\rm HI}$ fluctuations and the positive $b_f$
 starts to appear at the small scales. A transition scale, at which the $b_f$ transits from negative at larger scales to positive at
 smaller scales, increases with the neutral islands being ionized and the increasing contribution by HI in halos.

We also plot the $b_f$ after the completion of reionization in Fig.~\ref{fig:ps_HIbias}.
As expected, after the HI in the IGM gets all ionized, the remaining HI in halos positively correlate
with the underlying matter density, resulting in the positive bias at all scales after reionization.
Note that after reionization, the $b_f$ is basically a weighted halo bias on scales larger than
the cell size of our simulation. As we have neglected the rare halos with masses larger than the cell mass
and smoothed the HI density within cells, we have equivalently neglected the one-halo term contribution
to the power spectrum, and retained only the two-halo term on large scales \citep{Cooray2002},
which results in an under-estimate of the bias on small scales.
Also, we note that the halo model, as well as our method of populating simulation cells using the conditional
mass function, would under-estimate the halo bias on scales  $k\gtrsim 1 \,{\rm h^{-1}\, Mpc}$
as compared to that from N-body simulations. Both of these effects give rise to
the nearly scale-independent bias on the relevant scales.
Interestingly, the neutral fraction bias $b_f$ transits from fully negative to fully positive in a
very short time scale, which is a clear indication of the completion of reionization.

\begin{figure}
\centering
\subfigure[21 cm bias during early EoR]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=1.0\textwidth]{Bias_1Gpc_highz_deltat_total.pdf}
\end{minipage}%
}\\
\subfigure[21 cm bias during late EoR]{
\begin{minipage}[t]{0.5\textwidth}
\centering
\includegraphics[width=1.0\textwidth]{Bias_1Gpc_lowz_deltat_total.pdf}
\end{minipage}%
}%
\centering
\caption{The bias between the 21 cm brightness temperature and the dark matter density.
The top and bottom panels show results during the early and late stage of reionization, respectively.
}
\label{fig:bias2}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{Bias_igm_1Gpc_allz_deltat.pdf}
\includegraphics[width=0.5\textwidth]{Bias_hd_1Gpc_deltat.pdf}
\caption{The IGM (top panel) and halo (bottom panel) 21cm bias. }
\label{fig:deltahalobias}
\end{figure}

\subsection{The 21 cm bias $b_{21}$}

The evolution of the 21cm bias during the early and late stages of reionization is shown in Fig.~\ref{fig:bias2}.
The error bars for the $z=9.90$ and $z=9.00$ curves are derived by similar method as Fig. \ref{fig:ps2}.
Unlike the neutral fraction bias, the 21cm bias shows more complicated behavior,
especially in the early stage of EoR. The 21cm bias is always positive
on small scales, showing the dominance of the HI in halos.
However the neutral fraction bias is totally negative in the small scales at early EoR,
because the 21cm signal is weighted by local density, and the halo contribution is more apparent.

On large scales, the 21cm bias is positive at the beginning of reionization, then decreases to below zero and
becomes more and more negative during the early EoR, and then
increases again and becomes less and less negative during the late EoR.
During most of the EoR, there is a transition point at which the 21cm bias transits from
negative at large scales to positive at small scales, and this transition scale only shows an obvious
increase in the late EoR. Perhaps due to this shift of transition scale,  the bias is scale-dependent up to fairly large scales during the late EoR.
We also show the $b_{\rm 21}$ after the completion of reionization, which is a positive
horizontal line in the figure, similar to the $b_f$.

We plot the 21cm bias for HI in halos as well as in the IGM in Fig.~\ref{fig:deltahalobias}.
Similar to the cross-power spectra discussed in Sec. \ref{sec:ps}, on large scales the 21cm bias is dominated
by the IGM while on small scales it is dominated by halos. A critical scale, below which halos contribute more to
the 21cm bias than the IGM, increases with the decreasing redshift. Here we note that even considering only the
IGM contribution, the 21cm bias is still positive on the smallest scales. This is due to the density fluctuations in the neutral regions:
there are some relatively over-dense regions even in the under regions but not dense enough to collapse and produce ionizing photons.

\begin{figure}
\centering\
\includegraphics[width=0.5\textwidth]{retest_v4.pdf}
\caption{The neutral fraction bias at $z = 6.50$. The red and blue lines show the result of the default
simulation and higher-resolution simulation ($512^3$ cells in a box of 286 Mpc side length) respectively.
}
\label{fig:resolution1}
\end{figure}

We tested the resolution convergence of our simulation by using a simulation with higher resolution ($512^3$ cells) and
smaller box size (286 Mpc per side) while keeping other parameters the same as our fiducial simulation. The
density and ionization fields  are smoothed to the same resolution as our fiducial simulation, then the
halo HI content in each cell is assigned using the same model as described in section \ref{sec:massfunction}.
The neutral fraction bias of this higher resolution simulation and our fiducial simulation at the same redshift $z=6.50$ are shown
in Fig.~\ref{fig:resolution1}. We see that they agree with each other. More importantly, the transition scales at which
the $b_f$ changes the sign agrees with each other very well, indicating the robustness of our conclusions.

\section{Conclusions and discussions}
\label{sec:conclusions}

In this paper, we investigated the HI distribution thoughout the EoR, including the HI in the IGM from semi-numerical simulations, and the HI in halos from an empirical relation between HI mass and its host halo mass.
We focused on the bias of the HI distribution with respect to the underlying matter density distribution,
in terms of the neutral fraction bias and the 21cm brightness temperature bias.

We found that during the reionization stage when $x_{\rm HI}^{\rm IGM}\gtrsim0.05$, the neutral fraction bias is always negative at all scales. However the amplitude first increases, up to the maximum $\sim 3$ when $x_{\rm HI}^{\rm IGM}\sim0.5$,  then decreases. When $x_{\rm HI}^{\rm IGM}\sim0.05$, positive bias appears at the smallest scales.
 Since then the negative-to-positive transition scale keeps increasing as the reionization approaches to the end in a short time scale. It is a good indicator of the completion of the reionization process.

The 21cm bias, however, is more complicated than the neutral fraction bias. Compared with neutral fraction, the 21cm brightness temperature is weighted by local gas density, therefore more correlated with the dark matter. At the smallest scales, the 21cm bias is always positive throughout the EoR, due to the contribution from HI in small neutral islands and in halos.
At large scales, the 21cm bias is positive at the early EoR stage,  however its
amplitude decreases with decreasing IGM neutral fraction. At $x_{\rm HI}^{\rm IGM}\sim0.9$, the large scale 21cm bias transits from positive to negative. Since then the bias amplitude rises again, reaching its maximum absolute value
when the IGM is roughly at $x_{\rm HI}^{\rm IGM}\sim0.1$.
From then on, the amplitude of the large scale 21cm bias drops again. However, at the same time the small scale 21cm bias always keeps increasing, because the contribution from HI in halos becomes more and more important. As a result, the transition point at which the 21cm bias transits from positive to negative, keeps increasing. Finally the reionization completed and all 21cm bias becomes positive again.

In summary,  a transition of 21cm bias from positive
 to negative at large scales marks the starting of reionization,
while 21cm bias reverts negative to positive on large scales with
 the completion of reionization.

The 21cm fluctuation could be measured with the current or upcoming generation experiments such as LOFAR, MWA,
HERA or SKA-low. The dark matter distribution and its cross-correlation with 21cm studied here can not be measured directly,
but by cross-correlating the 21cm brightness field and some tracers of dark matter density, the 21cm bias can still be derived. The
21cm-dark matter cross correlation and bias is however more general than specific tracers. A number of high redshift observations
can be used to trace the large scale dark matter density,  for example the Lyman Break Galaxies (LBGs) and Ly$\alpha$
emitters (LAEs) derived from broadband or narrow band photometric observations
\citep{Dayal2012,Garel2015,Bouwens2015}. Of course, there will also some bias of the tracer sample with respect to the dark matter.
Indeed, \citet{Sobacchi2016} and \citet{Kubota2018} have investigated the detectability of 21cm-LAE cross-correlation
by combining the Subaru Hyper-Suprime Cam (HSC) Ultra-Deep field survey \citep{Aihara2018a,Aihara2018b} and
the upcoming 21cm survey with LOFAR, MWA, or SKA-low. Measurement of the cross-correlation with the
SKA-low is found very promising, and we expect the 21cm bias and its evolutionary features
could be determined via such measurement in the SKA era.

\section*{Acknowledgements}
We thank Renyue Cen,  Kwan Chuen Chan  and Francisco Villaescusa-Navarro for helpful discussions.
This work is supported by the the National Natural Science Foundation of China (NSFC) key project grant 11633004,
the NSFC-ISF joint research program No. 11761141012, the CAS Frontier Science Key Project QYZDJ-SSW-SLH017,
Chinese Academy of Sciences (CAS) Strategic Priority Research Program XDA15020200,   and
the MoST 2016YFE0100300. BY also acknowledges the support of  the CAS Pioneer Hundred Talents (Young Talents) program,
the NSFC grant 11653003, the NSFC-CAS  joint fund for space scientific satellites No. U1738125.
ITI was supported by the Science and Technology Facilities Council [grant numbers ST/I000976/1, ST/F002858/1
and ST/P000525/1];and The Southeast Physics Network (SEPNet).
We acknowledge that the results in this paper have been achieved using the PRACE
Research Infrastructure resources Curie based at the Trs Grand Centre de Calcul (TGCC) operated by CEA,
France and Marenostrum based in the Barcelona Supercomputing Center, Spain.The authors gratefully acknowledge
the Gauss Centre for Supercomputing e.V.(www.gauss-centre.eu) for funding this project by providing computing time
through the John von Neumann Institute for Computing
(NIC) on the GCS Supercomputers JURECA and JUWELS at Juelich Supercomputing Centre (JSC)

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


The 68th Venice International Film Festival, organised by La Biennale di Venezia, will be held on the Venice Lido from 31st August to 10th September 2011. Beside the "Venezia 68 - International competition", the Orizzonti sidebar presents a line of programming devoted to new tendencies in world cinema without distinction of genre or duration, presenting works that reflect the continual redefinition of filmmaking within the whole range of contemporary visual expression.
The 2010 Orizzonti line-up has featured brand new works from a number of renowned visual artists and film directors such as Doug Aitken, Douglas Gordon, Victor Alimpiev, Isaac Julien, Roee Rosen, Manoel De Oliveira, Ken Jacobs, Peter Tscherkassky, Semiconductor and Martin Arnold, as well as from several exciting new talents like Josh and Benny Safdie, Mauro Andrizzi, Xun Sun, Emily Richardson, Nicolas Provost or David O'Reilly, just to name a few.


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text:
Thomas P. McMahon, Esq. Jones & Keller, P.C.
Skilled Antitrust, Health Care And Complex Commercial Litigation Representation For Clients In Colorado And Nationwide.
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Antitrust Litigation and Counseling
Big Win in Federal Antitrust Trial
Tom McMahon and fellow Jones & Keller trial attorney Steve Long recently won a major jury verdict on behalf of Tom's client, Auraria Student Housing at the Regency, LLC (the "Regency"). The lawsuit charged that the defendant, Campus Village Apartments, LLC ("Campus Village"), conspired with the University of Colorado Denver ("UCD") to monopolize the rental to UCD freshmen of privately-owned and operated off-campus student housing in violation of Section 2 of the Sherman Antitrust Act.
Following 4½ days of testimony, the Denver federal court jury returned its verdict in the unheard-of span of 48 minutes. After being trebled pursuant to federal antitrust law, the judgment amounts to $9,783,000. In addition, the Regency is entitled to a statutorily-mandated award of attorneys' fees and costs of suit, which will add significantly to the Regency's total recovery.
Click here for the Denver Post's article on the case.
Colorado Federal Court Denies Defendant's Summary Judgment Attempt in Antitrust Case
Tom McMahon recently obtained a significant ruling in a cutting-edge federal antitrust case in Denver. Tom represents the Regency, a facility providing dedicated student housing for the three schools at the Auraria Campus in downtown Denver. The Regency is suing a competitor, Campus Village Apartments, for conspiring with the University of Colorado Denver to monopolize the provision of student housing to UCD freshmen by requiring them to live at Campus Village. Students are deprived of the choice of where to live, and forced to pay higher prices as a result. The U.S. District Court recently denied Campus Village's motion for summary judgment seeking to have the lawsuit dismissed. The case will now proceed to trial, which is scheduled for January 2015.
Montana Trial Court Ruling Holds Defendant Hospital Liable to Physician
Tom McMahon recently obtained a unique and significant ruling in a major health care case in Montana. Tom represents a physician with 33 years of experience who is suing a hospital for improperly ending his career as an ob/gyn. In an extremely rare move, the trial judge ruled as a matter of law that the hospital is liable to the physician for beaching its contract with him. Now the late August jury trial will focus primarily on damages, which are expected to amount to seven or eight figures. Rauh v. Holy Rosary Healthcare, Cause No. DV 2011-41 (Mont. 16th Jdcl. Dist., Custer Cnty., May 22, 2013)
U.S. Tenth Circuit Dismisses Private Defendant's Appeal Claiming Antitrust Immunity February 11, 2013
In an antitrust decision of national significance, on January 4, 2013 Jones & Keller senior litigator Tom McMahon won a favorable ruling from the U.S. Court of Appeals for the Tenth Circuit in Denver. The appellate court held that a private defendant may not invoke the "collateral order" doctrine to immediately appeal a trial court's ruling that the defendant does not have state action immunity from the antitrust laws. The case is Auraria Student Housing at the Regency, LLC v. Campus Village Apartments. LLC, ___ 703-F.3d ___1147, (10th Cir. 2013).
In the fall of 2010 Jones & Keller filed suit in U.S. District Court in Denver on behalf of its client, the Regency. The complaint alleged that defendant Campus Village had conspired with the University of Colorado-Denver ("UCD") to monopolize private, off-campus dedicated student housing apartment facilities for the Auraria Higher Education Center in violation of Section 2 of the Sherman Act, 15 U.S.C. §2. According to the complaint, the two agreed that UCD would require most of its full-time students to live at Campus Village's apartments for their first two semesters, rather than being able to live at the Regency or elsewhere. As a result, students paid more and received less at Campus Village and the Regency lost business.
Campus Village moved to dismiss the complaint, asserting that under the doctrine of Parker v. Brown, 317 U.S. 341 (1943), it had state action immunity from the antitrust laws. Jones & Keller opposed that on behalf of the Regency, relying heavily on the Tenth Circuit's then-recent decision in Kay Elec. Co-op v. City of Newkirk, 647 F.3d 1039 (10th Cir. 2011). In late 2011 the trial court denied the motion. 825 F.Supp.2d 1072 (D.Colo. 2011). Campus Village then filed an immediate appeal, asserting that it was entitled to do so under the collateral order doctrine of Cohen v. Beneficial Indus. Loan Corp., 337 U.S. 541 (1949), and re-asserting entitlement to state action immunity.
On January 4, 2013, the Tenth Circuit rejected the appeal. It noted that a split exists among federal appellate courts regarding whether the denial of state action immunity prior to trial is immediately appealable as a collateral order. The U.S. Courts of Appeals for the Fourth and Sixth Circuits have held it is not. See S.C. State Bd. of Dentistry v. FTC, 455 F. 3d 436 (4th Cir. 2006); Huron Valley Hosp., Inc. v. City of Pontiac, 792 F.2d 563 (6th Cir. 1986). Those for the Fifth and Eleventh Circuits have held, conversely, that it is. See Martin v. Mem'l Hosp., 86 F.3d 1391 (5th Cir. 1996); Commuter Transp. Sys., Inc. v. Hillsborough Cnty. Aviation Auth., 801 F.2d 1286 (11th Cir. 1986).
The Tenth Circuit emphasized, however, that even the Fifth Circuit does not allow privatedefendants to utilize the collateral order doctrine as a vehicle for immediately appealing the denial of state action immunity. See Acoustic Sys., Inc. v. Wenger Corp., 207 F.3d 287 (5th Cir. 2000), pointing out that immunity concerns regarding governmental defendants simply aren't implicated where a private party is the entity claiming state action immunity. Consequently, the Tenth Circuit dismissed Campus Village's appeal without even needing to address the underlying state action immunity issue.
The case now returns to the district court for trial.
Auraria Student Housing at the Regency, LLC v. Campus Village Apartments, LLC, Case No. 10-cv-2516 - WJM-KLM (D. Colo. Sep. 8, 2014)
Appellate Victory in Health Care Case of First Impression
In a case of first impression under the 36-year old state Professional Review Act governing physicians, Jones & Keller senior litigator Tom McMahon has won a precedent-establishing victory in the Colorado appellate courts that will benefit doctors throughout Colorado. The Act provides that, as a general rule, peer review materials are privileged and not subject to subpoena or discovery in civil lawsuits. However, it makes an exception for a physician in the course of an appeal during a peer review proceeding involving the physician, and again in a subsequent judicial review suit brought by the physician once the peer review proceeding is complete.
In the case handled by Tom, he subpoenaed peer review records on behalf of his physician client at both stages. During the peer review appeal, the hospital refused to produce the subpoenaed records. Then, on judicial review, the hospital persuaded the lower court to quash the second subpoena. The Court of Appeals held that the physician had a clear statutory right to the materials in the course of his peer review appeal, and reversed the lower court on that basis alone. Accordingly, it did not even have to address the lower court's action in failing to uphold the second subpoena - although the result would undoubtedly have been the same. Crow v. Penrose-St. Francis Healthcare Sys.,292 P.3d 1018 (Colo. App. 2012). The Colorado Supreme Court then refused to accept the hospital's attempt at a further appeal.
This is the latest victory Tom has obtained in the Colorado appellate courts on behalf of the same physician client against the same hospital. In 2010 the appellate court first reversed the lower court, upholding the physician's right to sue the hospital for damages over the faulty peer review process as soon as that administrative proceeding was completed. Crow v. Penrose-St. Francis Healthcare Sys., 2010 WL3169839 (Colo. App. 2010).
Together, these appellate victories do much to enable Colorado physicians to protect themselves when they become involved in peer review proceedings with hospitals.
Thomas P. McMahon
Contact Thomas P. McMahon, Esq. For An Initial Consultation
Attorney Thomas P. McMahon, Esq., of Jones & Keller, P.C., serves clients in Denver, statewide in Colorado and nationally.
© 2020 by Jones & Keller, P.C. All rights reserved. Disclaimer | Site Map

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text:
Michigan Wolverines vs. Notre Dame Fighting Irish NCAA betting tips
Betting Planet > Sports Betting Tips > Michigan Wolverines vs. Notre Dame Fighting Irish NCAA betting tips
By: Jason G
Michigan Wolverines vs. Notre Dame Fighting Irish
Notre Dame Stadium Notre Dame, Indiana, 7:30 PM EST Saturday September 1, 2018
Betting Line: Notre Dame -1
Over/Under: 46.5 points
The Irish and the Wolverines have a great rivalry, but they have not met since the 2014 season. They renew that heated NCAA rivalry this Saturday where Notre Dame is a very slight home favorite at Bovada.
Michigan has won six of their last nine games facing Notre Dame and they also 6-3 in that span.
In the AP poll Notre Dame is the 12th ranked teams in the nation and Michigan ranks 14th.
In some key head-to-head betting trends the home team is 4-0 ATS in the last four games between these teams and the underdog is 11-5 ATS in the last 16 meetings.
Michigan looks to get back into the elite of college football after a disappointing last season. They began 8-2, but they lost their last three games including losing to South Carolina in the Outback Bowl. The Wolverines return 16 starters, but one of the key players was not on their squad last season. Shea Patterson transferred from Ole Miss and last season he passed for 2,259 yards with 17 TD and nine TD for the Rebels.
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The Wolverines only ranked 91st in the nation last season in total offense, but they hope Patterson can help change that along with returning RB's Karon Hidgon and Chris Evans. Last season Hidgon rushed for 994 yards averaging a legit 6.1 yards per carry and Evans chimed in for 685 rushing yards. There is some talent in the WR corps, but they need some guys to step up. Grant Perry is back, but while leading the team last season he only had 307 yards with one TD.
Michigan's D was the strength of the team last season ranking 3rd in the nation. They return nine starters and should be great on that side of the ball again. The key for the Wolverines will be Patterson and the offense and if they can move the chains they will be hard to beat with the D they have, especially in the secondary.
Notre Dame finished 10-3 least season beating LSU in the Citrus Bowl. As usual the Fighting Irish played a killer schedule and they were 3-3 facing top 25 teams.
Duel threat QB Brandon Winbush is back under center for Notre Dame and last season he passed for 1,870 yards with 16 TD and six picks and also was the team's 2nd leading rusher with 803 yards and 14 TD. Winbush has a decent WR corps, but the Irish did lose their top WR from last season, but he is not a pure passer, which may hurt facing Michigan, who ranked #1 in the nation last season defending the pass.
Lead RB Josh Adams is gone, as well as last season's 3rd leading rusher, and the lead guy coming back is Dexter Williams, who rushed for 360 yards last season. Winbush needs help from the WR's and RB's, as he cannot do it all.
Notre Dame ranked a decent 46th in the nation last season on defense, but may be better this season. Te'von Coney leads the LB unit, Drue Tranquill is a S/LB hybrid, who is a monster, and CB Julian Love may have an All-American season with the talent he has. The D may have to really play well if the offense struggles to move the ball on a great Michigan defensive unit.
Michigan betting trends
Michigan is 1-3-1 ATS in their last 5 road games
Michigan is 1-5 ATS in their last 6 non-conference games
Michigan has an Over record of 11-4 in their last 15 road games
Notre Dame betting trends
Notre Dame is 1-4 ATS in their last 5 games
Notre Dame is 1-4 ATS in their last 5 games against Big 10 teams
Notre Dame has an Under record of 4-0 in their last 4 games
Michigan Wolverines vs. Notre Dame Fighting Irish betting picks
Notre Dame is at home and their D may be a very good one this season, but this game belongs to Michigan.
Patterson and the offense will have a decent game, but with the Wolverines having the defense they do that will be more than enough. This game will not feature a ton of points and Michigan will get the win on the road in this season opener.
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text:
Non 1001 Book Review: Dark Pines by Will Dean
Dark Pines by Will Dean
Reviewed by: Book Worm
Rating: [★★★★★]
This ARC was provided by One World Publications (via NetGalley) in exchange for an honest review.
Synopsis from Goodreads: An isolated Swedish town. A deaf reporter terrified of nature. A dense spruce forest overdue for harvest. A pair of eyeless hunters found murdered in the woods.
It's week one of the Swedish elk hunt and the sound of gunfire is everywhere. When Tuva Moodyson investigates the story that could make her career she stumbles on a web of secrets that knit Gavrik town together. Are the latest murders connected to the Medusa killings twenty years ago? Is someone following her? Why take the eyes? Tuva must face her demons and venture deep into the woods to stop the killer and write the story. And then get the hell out of Gavrik.
BookWorm's Thoughts: This is a fantastic first book in what I hope proves to be a long and fantastic series, book 2 is due to be published next year and I am super excited about this.
I would class this as a murder mystery story as opposed to a chiller/thriller and trust me that is no bad thing, however due to the nature of the story there is not much you can say in a review without giving away spoilers so you are just going to have to bear with me while I gush over all the things I loved about this book.
The first thing I love is Tuva Moodyson. Tuva is a young bisexual deaf woman working as a reporter, she has left the bright lights of London to return to Sweden to be close to her dying mother. Tuva is scared of nature but is facing her fears, she is at home with her deafness while also accepting that it sets her apart from other people, she is a single woman doing what she wants to do, she is a reporter who is actually interested in the truth and the people behind the headlines in short Tuva rocks. I love the way Tuva's deafness is very much a part of her story from her vibrating pillow alarm clock (genius) to the way she must always be prepared for the battery running out in her hearing aid.
The second thing I love is the villagers. Each villager is distinct and unusual in their own way, ok most of them are eccentric and perhaps other readers might find this stretches credulity but me, I loved them.
Utgard forest. The forest is very much a character in this book not just a setting. It provides the murder scenes, it provides uncertainty and fear, it also provides nature in the form of mice, elks, mosquitos and ticks.
Please indulge me while I share this beautiful description on how wool makes Tuva feel:
"I reach back awkwardly and pull the red yarn out of my backpack. It feels like Mum before Dad died; like Mum before she gave up all her hobbies; her bridge and knitting and backing and birdwatching; before she quit her job as an optician, before she gave up on life, before she gave up on me. The soft wool, springy in my fingers, feels like the good years before everything changed. It feels safe."
Who would enjoy this: Well you may guess from my review that I think everyone should read this but if I have to get specific I would say this is a book for those who like slower paced murder mysteries where character study is a big part of the story and where there is not too much blood and gore involved.
We want to hear from you! Have you read this book? What did you think?
Margaret Atwood Announces The Handmaid's Tale Sequel
Is this the most exciting bookish news this year?
Non 1001 Book Review: Salvage the Bones by Jesmyn Ward
What happens when the lives of a poor family in Mississippi clash with hurricane Katrina?
Non 1001 Book Review: The Line Becomes a River Francisco Cantú
The Line Becomes a River by Francisco Cantú
Rating: [★★★★]
Find it here: [jen will add amazon link]
A timely look at the immigration situation between Mexico and the USA.
Non 1001 Book Review: Do Not Disturb by Claire Douglas
The Labyrinth of the Spirits by Carlos Ruiz Zafon
This ARC was provided by Orion Publishing Group (via NetGalley) in exchange for an honest review.
Synopsis from Amazon: As a child, Daniel Sempere discovered among the passageways of the Cemetery of Forgotten Books an extraordinary novel that would change the course of his life. Now a young man in the Barcelona of the late 1950s, Daniel runs the Sempere & Sons bookshop and enjoys a seemingly fulfilling life with his loving wife and son. Yet the mystery surrounding the death of his mother continues to plague his soul despite the moving efforts of his wife Bea and his faithful friend Fermín to save him.
Just when Daniel believes he is close to solving this enigma, a conspiracy more sinister than he could have imagined spreads its tentacles from the hellish regime. That is when Alicia Gris appears, a soul born out of the nightmare of the war. She is the one who will lead Daniel to the edge of the abyss and reveal the secret history of his family, although at a terrifying price.
The Labyrinth of the Spirits is an electrifying tale of passion, intrigue and adventure. Within its haunting pages Carlos Ruiz Zafón masterfully weaves together plots and subplots in an intricate and intensely imagined homage to books, the art of storytelling and that magical bridge between literature and our lives.
Non 1001 Book Review: Vox by Christina Dalcher
Vox by Christina Dalcher
This ARC was provided by HQ (via NetGalley) in exchange for an honest review.
Synopsis from Goodreads: Set in an America where half the population has been silenced, VOX is the harrowing, unforgettable story of what one woman will do to protect herself and her daughter.
On the day the government decrees that women are no longer allowed more than 100 words daily, Dr. Jean McClellan is in denial—this can't happen here. Not in America. Not to her.
This is just the beginning.
Soon women can no longer hold jobs. Girls are no longer taught to read or write. Females no longer have a voice. Before, the average person spoke sixteen thousand words a day, but now women only have one hundred to make themselves heard.
But this is not the end.
For herself, her daughter, and every woman silenced, Jean will reclaim her voice.
Non 1001 Book Review: I Still Dream by James Smythe
I Still Dream by James Smythe
This ARC was provided by Harper Collins UK (via NetGalley) in exchange for an honest review.
Synopsis from Goodreads: 1997.
17-year-old Laura Bow has invented a rudimentary artificial intelligence, and named it Organon. At first it's intended to be a sounding-board for her teenage frustrations, a surrogate best friend; but as she grows older, Organon grows with her.
As the world becomes a very different place, technology changes the way we live, love and die; massive corporations develop rival intelligences to Laura's, ones without safety barriers or morals; and Laura is forced to decide whether or not to share her creation with the world. If it falls into the wrong hands, she knows, its power could be abused. But what if Organon is the only thing that can stop humanity from hurting itself irreparably?
I Still Dream is a powerful tale of love, loss and hope; a frightening, heartbreakingly human look at who we are now–and who we can be, if we only allow ourselves.
Non 1001 Book Review: It Ends with You by S K Wright
It Ends with You by S K Wright
Rating: [★★★]
This ARC was provided by Little Brown Book Group UK (via NetGalley) in exchange for an honest review.
Synopsis from Goodreads: 'If I'd told the truth, it would have been fiction'
Everyone loves Eva. Beautiful, bright, fun, generous – she's perfect.
So when her dead body is found in a ditch in the local woods the only thing anyone wants to know is: Who could have done this?
It has to be Luke, her boyfriend. He has the motive, the means, the opportunity and he's no stranger to the police.
Even though the picture is incomplete, the pieces fit. But as time passes, stories change.
Told from six narrative strands, this cleverly woven and utterly compulsive novel challenges preconceptions; makes you second, third and fourth guess yourself; and holds an uncomfortable mirror up to the way societies and systems treat those they perceive to be on the outside.
October Roundup
As Jen is really busy in the real world you are stuck with me for a little while. I apologise in advance for not being as on the ball in terms of updates and formatting as Jen usually is but rest assured normal service will resume soon.


You are visiting the placeholder page for Bill Barker. This page is here because someone used our placeholder utility to look for Bill Barker. We created this page automatically in hopes Bill Barker would find it. If you are not Bill Barker, but are an alumni of Clover Park High School, register on this site for free now.


Concrete is a very durable material that is used, not just outside for driveways and walkways, but also inside for basements and subfloors. As durable as it is, concrete can become weathered and pitted, even indoors, and this can look unsightly on any surface. You don't need to put up with unsightly walkways, driveways, garage floors, and basement walls when the concrete gets a bit old, and you don't need to necessarily tear it up and replace the material either. Note a few quick tips for restoring the look of your home's concrete surfaces, and then discuss your options with a contractor.
Grinding doesn't refer to actually grinding up concrete into dust, but refers to grinding the top layer of concrete so that it becomes smooth; this is similar to buffing a glass surface. Grinding your concrete surface can remove those pitted areas and small cracks; this can make your concrete look better and can also make it safer for walking, as you're less likely to trip on chips and cracks when you choose concrete grinding. Grinding is a popular choice for garage floors and basement floors, as this smooth surface can make the floors seem more appropriate for indoors and make them look less industrial. If you have any questions about grinding, consider contacting a local concrete cutting specialist, such as Kwik Cut.
Did you know that concrete could be painted? It's good to choose a paint meant specifically for concrete or cement so you know it will adhere properly without peeling off, but this can make your basement walls and floor or garage floor look fresh and new; you can even paint your home's driveway to coordinate with your house color.
Stamping refers to putting a type of paint or coating on the concrete to make it look like another material, such as stone. This is a good choice for walkways, patios, and other areas where you want a decorative look.
Aggregate refers to a material that you mix with concrete to make it bumpier and to give it a certain texture. Aggregate can be colored pebbles or smooth glass. If your original concrete did not have aggregate added, you might have a new layer of concrete put over the top of your old concrete with an aggregate added in. This can give the area texture and color; it can also make driveways and walkways safer, as the aggregate adds traction for when the concrete gets wet or icy.


E-mail written 31 Jan 2008 to Warren Culpepper from Cheryl Sue Culpepper (#23491), e-mail address.
Cory Dalton Culpepper, Male, born __ 1987 in Gray Co., Texas, child of Myron Jeffrey Culpepper and Lisa Gayle Drake.
Father* John Harry Culpepper Jr.
Amanda Dolores Culpepper, Female, born __ 1981 in Dallas Co., Texas, child of Johnny Harry Culpepper, II and Darla Lynn Cleveland.
Joe Brian Culpepper, Male, born __ 1985 in Dallas Co., Texas, child of Johnny Harry Culpepper, II and Darla Lynn Cleveland.
James Austin Culpepper, Male, born __ 1981 in Dallas Co., Texas, child of Carroll Dee Culpepper and Connie Lou Ott.
Connie Lou Ott, born 3 Feb 1959 in Dallas Co., TX, daughter of Charles Adolph Ott and Mildred Mae Reynolds.
Carroll D Culpepper, 20, married Connie L Ott, 18, on 7 Jul 1977 in Dallas Co., TX.
James Culpepper is the drummer of the heavy rock quintet, Flyleaf. Their eponymous debut album, Flyleaf, went platinum in 2005 after selling more than one million copies. Their sophomore album, Memento Mori was released on November 10, 2009.