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Jason Momoa Movies
Aquaman CAM
Director: James Wan
Actor: Jason Momoa, Amber Heard, Willem Dafoe, Amber Heard, Patrick Wilson, Dolph Lundgren, Yahya Abdul-Mateen II, Nicole Kidman, Temuera Morrison, Ludi Lin
Braven HD
A logger defends his family from a group of dangerous drug runners.
Director: Lin Oeding
Actor: Jason Momoa, Stephen Lang, Garret Dillahunt, Zahn McClarnon, Jill Wagner, Brendan Fletcher, Sala Baker, Teach Grant, Fraser Aitcheson, James Harvey Ward
Bullet to the Head HD
After watching their respective partners die, a cop and a hitman form an alliance in order to bring down their common enemy.
Director: Walter Hill
Actor: Sylvester Stallone, Sung Kang, Sarah Shahi, Adewale Akinnuoye-Agbaje, Jason Momoa, Christian Slater, Jon Seda, Holt McCallany, Brian Van Holt, Weronika Rosati
Conan the Barbarian HD
A vengeful barbarian warrior sets off to get his revenge on the evil warlord who attacked his village and murdered his father when he was a boy.
Director: Marcus Nispel
Actor: Jason Momoa, Stephen Lang, Rachel Nichols, Ron Perlman, Rose McGowan, Bob Sapp, Leo Howard, Steven O'Donnell, Nonso Anozie, Raad Rawi
Frontier - Season 3
Frontier - Season 3 HD
Follows Declan Harp, a part-Irish, part-Native American outlaw who is campaigning to breach the Hudson's Bay Company's monopoly on the fur trade in Canada.
Director: Rob Blackie
Actor: Jason Momoa, Landon Liboiron, Alun Armstrong, Jessica Matten, Zoe Boyle, Lyla Porter-Follows, Allan Hawco, Christian McKay, William Belleau, Evan Jonigkeit
Justice League HD
Fueled by his restored faith in humanity and inspired by Superman's selfless act, Bruce Wayne enlists the help of his newfound ally, Diana Prince, to face an ..
Actor: Ben Affleck, Henry Cavill, Gal Gadot, Amy Adams, Ezra Miller, Jason Momoa, Ray Fisher, Jeremy Irons, Diane Lane, Connie Nielsen
Once Upon a Time in Venice HD
A Los Angeles detective seeks out the ruthless gang that stole his dog.
Genre: Action, Comedy, Thriller
Director: Mark Cullen
Actor: Bruce Willis, Jason Momoa, John Goodman, Thomas Middleditch, Famke Janssen, Elisabeth Röhm, Adam Goldberg, Wood Harris, Emily Robinson, Kal Penn
Sugar Mountain HD
Two brothers, down on their luck, fake a disappearance in the Alaskan wilderness so they'll have a great survival story to sell, but the hoax turns out to be ..
Director: Richard Gray
Actor: Jason Momoa, Cary Elwes, Melora Walters, Anna Hutchison, John Karna, Drew Roy, Haley Webb, Shane Coffey, Steve Mouzakis
The Lego Movie 2: The Second Part CAM
It's been five years since everything was awesome and the citizens are facing a huge new threat: LEGO DUPLO® invaders from outer space, wrecking everything f..
Genre: Animation, Family, Action, Adventure, Comedy, Sci-Fi, Fantasy
Director: Mike Mitchell
Actor: Chris Pratt, Elizabeth Banks, Will Arnett, Tiffany Haddish, Stephanie Beatriz, Alison Brie, Nick Offerman, Charlie Day, Jason Momoa, Channing Tatum
Wolves HD
A boy is trying to find out about his family history and stumbles upon a town of lycans.
Country: France, Canada
Genre: Action, Fantasy, Horror
Director: David Hayter
Actor: Lucas Till, Jason Momoa, John Pyper-Ferguson, Stephen McHattie, Merritt Patterson, Janet-Laine Green, Melanie Scrofano, Kaitlyn Wong, Adam Butcher, Philip Maurice Hayes

redpajama_set_name: RedPajamaCommonCrawl


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Summer of Darkness: Investigating Film Noir
Jean-Paul Goddard as an Extension of Film Noir
By dr4gonhunt3r,
June 15, 2015 in Summer of Darkness: Investigating Film Noir
dr4gonhunt3r
I have been thinking, as I have been watching the last several films this weekend, about the morality of the diegesis of the Film Noir movement films (yes, I consider them a movement which created a style and genre within the decades it was active, much like movements in the the more stationary visual arts). There has been talk of the protagonists being morally grey persons trying to navigate a corrupt world (I paraphrase) in the notes and lecture. In this sense Film Noir could be thought of as a mirror of the modernist view that the rules of morality have been broken, or are widely not followed. Hence the rampant violence, greed, sex, and general vice. The protagonists are, by comparison to the world at large, heros by simply following the rules some of the time.
The next challenge for me is how to relate this to the works of Jean-Paul Goddard in the 60's, which are arguably part of the evolution from Film Noir in the 50's. Goddard is definitely influenced by Film Noir and heavily uses elements of the movement. There is gratuitous violence (e.g. bloody car-crash scenes litter the sides of the road in Pierrot le Fou), sex, light play in the style of Noir Expressionism, a focus on how the protagonist will react rather than the resolution of a mystery or plot. Even so, there seems to be a shift in thought from the social and moral rules being ignored, to a world where the rules don't exist or have ceased to make sense. This, I feel, comes from the separate influence of Avant Garde film (I consider this film thought of as art work and self-referential rather than entertainment) which serves to make several of his films surreal and/or non-sensical, but within the work as a whole represents the new sentiments of people in this era towards the world they live in.
I also wonder if this shift in thought, if that is indeed the case, would be related to the Korean and Vietnam wars which were occurring in the 50's and 60's.
Does anyone else have thoughts on classifying Film Noir as a movement like other visual arts, looking at Film Noir as a commentary on the view of the world via social rules, and whether or not Goddard can be considered a natural progression from that?
Also, does anyone know of other films that would support this hypothesis?
PiercingMildred
LocationAmerica
I definitely believe that the filmmakers of the French "New Wave" were making film noir. Think 'Breathless.'
rrrick
LocationNetherlands
The next challenge for me is how to relate this to the works of Jean-Paul Goddard in the 60's,
Just a small correction, it's Jean-Luc Godard
Not just him, but other French directors part of, or linked to the Nouvelle Vague made Noir-ish crime films. Truffaut's SHOOT THE PIANO PLAYER, Becker NE TOUCHE PAS LE GRISBI, Melville's BOB LE FLAMBEUR, Dassin's RIFIFI and Malle's ELEVATOR TO THE GALLOWS are good examples.
Godard is without a doubt my 'favorite' director, as in that his films set me on the path of really going deep into cinema, and try and understand it as an art form. But at the same time, I'm not even going close to saying that I understand his films, his theories and motivations. It's obvious American films, and especially crime films have influenced him greatly, but how and to what extent is essentially still mystifying to me. The guy remains an enigma.
Not just him, but other French directors part of, or linked to the Nouvelle Vague made Noir-ish crime films. Truffaut's SHOOT THE PIANO PLAYER, Becker NE TOUCHE PAS LE GRISBI, Melville's BOB LE FLAMBUER, Dassin's RIFIFI and Malle's ELEVATOR TO THE GALLOWS are good examples.
Godard is without a doubt my 'favorite' director, as in that his films set me on the path of really going deep into cinema, and try and understand it as an art form.
Boy, do I feel embarrassed. ^^;;; I blame temporary alien hand syndrome.
Godard is one of my favorite directors for the same reason. I have a Studio Art background, and we studied him in a very art film context. Much of how I read his films is in exploring film as an art medium. I will definitely have to take a look at these other films! Thanks for the suggestions!
It's been a while since I've seen Breathless, but it is one of Goddard's earlier works and much more conventional in it's format and style than some of his later works. It does have a very Film Noir style to it, but from what I can recall it seemed lighter, not as full of corruption and vice, but I would have to re-watch it to say anything for sure. Do you have specific examples of why you think it is a Film Noir film rather than part of a movement related to, but not part of, Film Noir?
Thanks for both of your input!
I suppose because the course is focused on FIlm Noir itself, and I take the viewpoint of Noir being a movement, the context of Noir, not only during the making of these films, but also in the years before and after as well as in other parts of the world are of interest to me. On that note, has anyone else seen the documentary on the entire history of Cinema across the world? I forget the name of it, but it was on Netflix a few months ago and came in a miniseries like format.
On that note, has anyone else seen the documentary on the entire history of Cinema across the world? I forget the name of it, but it was on Netflix a few months ago and came in a miniseries like format.
THE STORY OF FILM, 10 part documentary by Mark Cousins. He takes a pretty radical approach to film history, challenging the notion that Hollywood 'classics' are classics in the true sense. I loved it, and it really set me on a path to widen my film horizon even further.
Jean-Paul Belmond's character is certainly the doomed protagonist and Jean Seburg is the femme fatal in that she is his lover n trusted confidant but imitably gives him up to the police. I'd have to watch the film again myself but if I remember correctly there were lots of absurd/surrealistic scenes and dioalogue, cinematographic chiaroscuro and unusual camera angles.
Godard is testing and stretching the limits of cinema as a narrative medium in BREATHLESS. It has many moment where he breaks the then standard cinematic conventions, like characters speaking directly into the camera, very long takes, and most famously, the use of jump cuts. Belmondo's character is modeled after Humphrey Bogart. In one scene Belmondo goes to the cinema and sees a couple of stills from a Bogart movie. He watches admiringly and then brushes his lips with his thumb like Bogart often did in his films. My guess is BREATHLESS is basically a humorous pastiche of American gangster films, but also a serious attempt to put cinema on the map as a (possibly radical) art form with its own unique characteristics and possibilities.
But maybe I've got it all wrong. Godard is an enigma.
Yup. The scenes with him thumbing his lip are forever imbedded in me mind.


I am excited to announce that the first of the four girls (who were pregnant in Sharon's wedding) had her baby! No, the births apparently are not going to occur in chronological order, which is good news for me since I should be last....but as always, I do not follow the trends of the other three so I am guessing I will be the last to have my baby. The first girl, Michele, had a healthy little boy! The exciting news is the person who was supposed to be first, had her water break last night! So hopefully there will be another little miracle soon!
I am hoping that my baby will come a little early like both of theirs (again I do not anticipate this, but a girl can dream!). My boss informed me to not get my hopes up that the baby would be late because it is my first baby. She said not to get my hopes up because I will be highly disappointed when my due date comes and goes and there is still no baby. My plan? I plan to work out everyday...in the pool if my gym will allow and walk every day once the doctor says it's safe for the baby to be born. I believe this is typically three weeks before the due date. I know it may not make her come any earlier, but hopefully it will keep me from desperation snacking and gaining unneeded and unwanted extra pounds that many moms keep warning me about. I like to be in control, and it's the only thing I can think of to do that will at least give me the illusion of a little control over my out of control body! My mom thinks Gabby will come two weeks early so please pray that she is right and that everything goes as smoothly and easily as possible.


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Vote for one of the nominated Chef's Gardens from the list below. All nominees are from the larger DC metropolitan region, including Northern Virginia and Maryland, and have developed a model cooking garden whether its at a farm, on a city lot or building rooftop.
Keith Cabot's garden above Evening Star Cafe is 1,360 square feet and yields enough produce to sustain 60-70% of his menu during peak season. Keith works closely with a part time gardener, Jonathan Stark, to start beds of seeds under grow lights offsite. Once germinated, the beds are transplanted to Evening Star's rooftop garden – making the most of the space and taking advantage of every square foot. In the summertime, Keith and Jonathan are up on the roof harvesting every single day. In the summer they'll harvest tomatoes, basil, eggplant, shishito peppers, shiso, purple long beans, Israeli cucumbers, sour gherkins and more. The winter brings arugula, mixed lettuce, chicories, a lot more herb production, thyme, basil, rosemary, radishes, turnips, and more. Year-round herb patches yield lavender and rosemary for cocktail syrups, thyme, thai basil, sorrel, cutting celery, and hibiscus to name a few. The herbs get harvested every other day for garnishes. The size of the garden is large enough to sustain dishes on the menu so that Keith isn't supplementing with inferior product, yielding about 15-20 lbs of produce per week. In the summer, Keith shares his surplus with Rob Rubba (Executive Chef, Hazel), Tom Cardarelli (Executive Chef, Vermilion), and Nick Farrell (Spirits Manager, Vermilion and Iron Gate) so that nothing goes to waste. Keith composts mundane restaurant food waste like coffee grounds and shrimp shells for the soil.
Rob makes the best of his urban setting and gardens in four separate garden spaces, all within 5 blocks of his restaurant. He has two community garden plots, his own back garden at home and a patio garden at Garrison. For years, Rob has remained dedicated to seeking out organic gardening in the middle of D.C. because it not only inspires his cooking, but also allows him to meet his neighbors. He makes these small garden plots punch above their weight in his chef training program. Every stage-ist and extern who works in the Garrison kitchen has gardening responsibilities as part of their training. Rob believes that the foundation of every good cook, whether professional or amateur, should start with an appreciation for growing things, getting your hands dirty in the garden and tasting things fresh off the vine or out of the ground.
Urbana's rooftop has a 1,000 square foot garden tended by Chef Ethan and his staff. All produce is harvested for consumption at Urbana or at Hotel Palomar events. The Urbana team sourced 1,000 pounds of mixed produce in 2015 and 1,500 pounds of mixed produce in 2016. The quality and freshness of the products can't be beat. Chef Ethan can pick fresh herbs and vegetables in the morning and use them on pizzas and pastas for dinner instead of using days-old ingredients from a purveyor. In the summer months, the modern Italian restaurant sources 100% of its basil supply from the rooftop which in 2015 and 2016 yielded a total of 500 pounds. Urbana's Lead Bartender Andrea Tateosian sources rooftop herbs for her Italian-leaning cocktail program as well. Last year's harvest savings are estimated at approximately $15,000. Chef Ethan also partners with FreshFarm's Foodprints program to bring cooking classes to DC Public Schools. Many of the ingredients used in these classes are sourced from Urbana's chef garden and the student-run garden at Francis Stevens School. Urbana was a recipient of Slow Food DC's Snail of Approval Award in 2016 as a result of its chef garden and general sustainability practices.


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Flames' winning spree ends in shutout loss to Canadiens
Wes Gilbertson
MONTREAL — The Calgary Flames' five-game winning streak?
C'est fini.
The Flames followed up their most emotional victory of the season with an absolute dud, lacking any sort of spark early en route to their first loss of 2020 — Monday's 2-0 blanking from the Montreal Canadiens at Bell Centre.
"This is twice this has happened to us after a big emotional game, where we've come flat the next game," groaned Flames interim head coach Geoff Ward, referring to Saturday's heated triumph over the Edmonton Oilers and the Battle of Alberta before that, too. "And it's the time of the year when we can't do that. We have to be prepared to play. I thought we weren't. We got out-battled, out-raced, out-competed, out-worked right from the very opening faceoff.
"We talked about it that (Monday) could potentially be a trap game in terms of not being ready to play and maybe sitting back in the last hockey game too much. But it's something that we have to rectify. This is part of learning to win. You know, when the game is over, it's over, and you have to get onto the next one. For whatever reason, we weren't prepared to go tonight from the drop of the puck. And as a result, we end up on the short end of the game."
While the Flames wasted an opportunity to pull two points ahead atop the Pacific Division standings, there was a sliver of good news Monday.
After looking a bit leaky in three straight outings, and then after a week-long layoff, go-to goalie David Rittich admitted he was feeling better about himself after his 35-save performance at Bell Centre.
If not for his efforts, the Flames might have been trailing by three or four at the first intermission.
Rittich had already turned aside 13 shots when Jordan Weal cashed a spinning shot at the 13:30 mark of the opening stanza for the would-be winner. At the opposite end, Carey Price had only faced two pucks up to that point.
"He was tremendous for us tonight," said Flames centre Mikael Backund of Rittich. "He kept us in the game in the first. It could have been a lot uglier than it was."
Echoed winger Johnny Gaudreau: "They could have taken the game away from us early, but he stood on his head and played really well for us."
Indeed, Rittich was Calgary's best-of-bunch.
Turns out, however, he needed to be perfect.
Price recorded 31 saves for the shutout, with more than half of those coming during a third-period push by the out-of-town team. For much of the night, it wasn't as even as the final shot tally would suggest.
Rust didn't seem to be an issue for Rittich, who had watched usual backup Cam Talbot log three straight starts — including Saturday's 4-3 win over the Oilers at the Saddledome.
The 27-year-old masked man flashed his right pad to thwart Habs captain Shea Weber on the opening shift in Montreal.
A few minutes later, he managed to get his glove on another blast from Weber, a three-time winner of the NHL's hardest shot competition.
His slate of saves also included a beauty blocker on Ryan Poehling and a string of stops on Jesperi Kotkaniemi, who had several whacks at a rebound on the power play.
"You know, I feel good when I get a lot of saves and a lot of things happening in front of me," Rittich said afterward. "It gave me a little bit of confidence, what I lost in the last three games. I felt good. I felt like myself. But still, we lost the game, and that's what really matters."
The Flames cranked up the pressure in the third, but the hosts added some insurance after an oopsie by Calgary's top defence pairing.
After a faceoff win in their own zone, captain Mark Giordano tried to push a pass to longtime sidekick TJ Brodie. They weren't on the same page, though, and Poehling claimed the loose puck and showed impressive patience before firing a forehand past a sprawling Rittich.
It was that kind of night for the Flames, who certainly didn't look like a crew that had rolled to five Ws in a row and just knocked off their arch-rivals.
"We can't say we were perfect in all five games, but we did enough to find ways to win," Ward said. "I thought in the Edmonton game the other night, we were real good. And then we come out tonight and we're flat. So we have to address that so it doesn't raise its head again."
Talbot's stingy stretch didn't go unnoticed. The 32-year-old was saluted Monday as the NHL's third star of the week after backstopping the crew from Calgary to three consecutive victories, posting a sparkling 1.67 goals-against average and .953 save percentage during that span … Edmonton Oilers tough guy Zack Kassian was dinged with a two-game suspension after thumping Flames alternate captain Matthew Tkachuk with several punches in Saturday's Battle of Alberta. Tkachuk wasn't willing to tussle, and the Flames buried the would-be game-winner on the ensuing power play … Flames winger Andrew Mangiapane marked a milestone Monday, hitting the 100-game plateau at the NHL level … Alexander Yelesin joined the Flames in Montreal, but the 23-year-old defenceman — freshly recalled from the American Hockey League's Stockton Heat — was a scratch against the Canadiens.
wgilbertson@postmedia.com
Twitter.com/WesGilbertson
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How much do Cornerstone Brands employees make? Glassdoor has salaries, wages, tips, bonuses, and hourly pay based upon employee reports and estimates.
See Cornerstone Brands Hourly Pay or Cornerstone Brands Bonuses.
Our Distribution Center held a luncheon for 31 of our associates that had perfect attendance in 2016! Seven of these associates have achieved this honor for 5 or more years! CONGRATULATIONS to of our associates that achieved the goal of Perfect!


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Gadgets > Games > COD: Modern Warfare Movie Trailer?
COD: Modern Warfare Movie Trailer?
By Radek Bonk on March 3rd, 2011
Last week, the website FindMakarov.com was discovered (or leaked) to various members of the video gaming community. The site contained a lone countdown clock, counting down to what many people believed would be the announcement of Modern Warfare 3, the next edition of the Call of Duty series.
However, the Call of Duty series owner Activision was quick to label it as a hoax and insisted the site had nothing to do with future games. The countdown clock expired and Activision was right … though we are left with more questions than answers.
What appeared on the site once the countdown was over was a rather impressive looking trailer for a Modern Warfare movie. Using plenty of the cut-scenes from the actual video game, the trailer brings the game to life in a way we've really not seen before.
We'd label it as a fan-made trailer, but it does raise the question of whether a real Call of Duty movie could be in the works in the near future, given the success of the franchise.
Christmas Electronics of Yore
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GEODIS, the logistics partner of Maxi Sport, has opened a new dedicated storage space at its Landriano warehouse in order to ensure end-to-end delivery for the sportswear retailer throughout Italy.
This new storage space of 5,000 sq m is located at the heart of the Landriano site. Approximately one third of the 800,000 pieces of sportswear handled each year is sold via e-commerce orders from the maxistore.com online site.
Furthermore, GEODIS provides a more flexible supply chain management to Maxi Sport to ensure management of seasonal peaks.
"Supporting the business of a leading customer like Maxi Sport drove us, once again, to search for new end-to-end solutions, especially in this sector where the care for the final product and smart logistics management are key elements" – says Francesco Cazzaniga, Contract Logistics Managing Director for GEODIS in Italy.


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Q: M3U8 parsing with NuGet package M3USharp I need to read in an m3u8 master playlist, the individual chunk playlists, and the individual binary data chunks.  I am just moving the data around, not doing any playbacks.
I'm using a NuGet package M3USharp to parse the master playlist, which gives me a list of streams.  From each individual stream, I can get each chuck playlist.  but I can not parse the chunk lists to get the individual chunks.  I can not find any examples showing how to do this with this package.
this is my code:
var content = getMasterFilePlaylist();
M3UFile m3u8File = M3UReader.Parse(content);

foreach(var stream in m3u8File.Streams)
{
     Console.WriteLine(stream.Path);

     // do stuff here...
}

But I can not find any examples for paring the chunk lists.
are there any other packages I should be using?

redpajama_set_name: RedPajamaStackExchange


I Have Crystals In My Ears?
As strange as it seems, everyone has microscopic crystals residing in their inner ears. These crystals are called Otoconia and are found in the Otolith organs, which are two pouches inside the vestibular system that are filled with fluid. The pouches are lined with small hairs and the small hairs are lined with the Otoconia. When the head tilts, the crystals attached to the hairs move through the ear fluid and send nerve signals to the brain.
"Wireless connectivity" is a hot topic in the world of hearing aids and we want to help you understand what it is, and whether it is, for you!
Virginia ENT has a new aesthetic laser, Sciton's Halo™ - Hybrid Fractional Laser (HFL). It's a fantastic new addition to our list of non-surgical aesthetic offerings. With the Halo HFL, we have a new option for maximizing results and minimizing downtime!
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When most people think of hearing loss, they may think of someone asking others to repeat themselves, or needing to turn up the volume on the TV. These are among the more common signs of hearing loss. But there are other symptoms of hearing loss that are less visible. Not all of them are easy to spot unless you know what you're looking for. What are these symptoms, and what should you do if you experience them?
You may have heard about the health benefits of a sinus rinse -- how it can keep your nose healthy and prevent sinus problems. But what is it?
In many cases, ear pain is caused by an infection of the ear canal. But did you know some ear pain may not be connected to ear-related problems at all? Many of these problems require a physician's knowledge to distinguish one problem from another. But here are a few other causes of ear pain you may not know about.
Hearing is vital to our quality of life. Hearing issues can affect so many facets of our lives, from employment to interpersonal relationships. People with hearing issues often end up avoiding or withdrawing from social situations because of the difficulty it can cause. And the more they withdraw, the less likely it is they will return to those social situations in the future.
Laryngitis is a common inflammatory condition of the larynx (or voice box). Much of the time laryngitis is painless, although some patients can experience pain. Laryngitis most often presents as voice hoarseness, frequent throat clearing, or a raspy or breathy voice. A sore throat and trouble swallowing may also occur.
Hearing Aid Cleaning - Are You Cleaning Them Correctly?
How often should you clean your hearing aids? Would you be surprised to learn you should clean them every day? Many hearing aid owners might not know that properly cleaning their hearing aids can lead to years of quality performance and long service.
Voice loss and hoarseness are common problems cared for in the otolaryngologist's (ENT) office on a daily basis. The frequency of these complaints does seem to increase in the winter months. It's likely that upper respiratory infections are playing a role in this seasonal increase.
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Here in Richmond, Virginia, there are several different resources for obtaining a hearing test, but the best place to go depends on your objectives in obtaining the hearing test. Here's a review of the different types of hearing tests offered.
You may have heard of platelet-rich plasma therapy (PRP), but you may not actually know much about it. What is PRP used for? Who can be a candidate for PRP? What should you do if you're interested in PRP?
Fall will hit Richmond before you know it -- and with that comes fall allergies. Allergy sufferers know all too well how autumn can worsen allergies. Fortunately, there are steps you can take to help mitigate the effects of seasonal allergies. In this article, we'll discuss the most common allergens that arrive with the autumn leaves, what you need to do now, and when to see a doctor or specialist.


text:
\section{Introduction}
\label{sec:intro}
Magnetic fields in the vicinity of supermassive black holes (SMBHs) are believed to be one of the most fundamental parameters governing the launch of relativistic jets \citep{blandford77} and generation of hot accretion disk coronae \citep{haardt91}. Various attempts have been made to measure magnetic fields at the center of active galactic nuclei \citep[AGNs;][]{gnedin2014,lopez2015,Marti-Vidal2015}. To date, however, magnetic fields in the inner accretion disk region at the scale of tens of Schwarzschild radii ($r_s$) have not been measured yet.

In the radio centimeter (cm) or longer wavelength regime, synchrotron radiation from AGN jets and/or galactic cosmic-ray particles dominate the emission, while extended galactic thermal dust emission dominates the millimeter (mm) radiation. It is theoretically predicted that there also exists radio synchrotron emission arising from accreting hot plasma, namely corona, near central SMBHs appearing in the mm band due to the strong synchrotron self-absorption (SSA) effect by the coronal component itself \citep{DiMatteo1997,laor2008,Veledina2011,inoue2014,Raginski:2016}.

Previous observations had presented inconclusive signs of a new component in the radio spectra of several Seyfert galaxies.  The putative new component -- so-called mm excess -- had been explored only in the short cm regime \citep{antonucci1988,barvainis1996} or a monochromatic mm band \citep{behar2015,Behar2018}.  Recently, a multi-band observation at 7 mm and longer wavelengths presented a possible sign for the existence of mm excess \citep{doi2016}.  Synchrotron emission from thermal hot plasma and free-free emission from surrounding ionized materials are found to be difficult to explain the putative mm-excess in terms of luminosity \citep{Field1993,laor2008,doi2016}. However, it is still inconclusive evidence because a paucity of multi-band data at shorter wavelengths. Investigation using conventional mm telescopes has been also hampered by the contamination of extended galactic emission.  Thus, the existence as well as physical origins of those excesses are still veiled in mystery.  High angular resolution and multi-band observations are required for the detection and understanding of compact coronal synchrotron emission \citep{inoue2014}.

By utilizing the Atacama Large Millimeter/submillimeter Array (ALMA), we have obtained new measurements for nearby radio-quiet Seyferts IC~4329A and NGC~985 at 12 frequency bands from 90~GHz up to 250~GHz. The observed radio emission is hardly contaminated by dust because of the sub-arcsec resolution of ALMA. We further analyzed archival cm data from the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA). In this paper, we report our new observational results.

This paper is organized as follows. In Section 2, we introduce our observations and data analysis. In Section 3, we present our results. Discussion and conclusion are given in Sections 4 and 5, respectively.

\section{Observations}
\label{sec:obs}

\subsection{Target objects}
IC~4329A is a southern Seyfert~1.2 galaxy at $z=0.0161$ \citep{wil91} whose central black hole mass is $\sim1.2\times10^8~M_\odot$ \citep{nik04,mar09}. The host galaxy is an edge-on spiral galaxy in a pair with IC~4329 separated by $\sim3$~arcmin. IC~4329A is one of the brightest X-ray Seyferts and shows a typical spectrum of radio-quiet Seyferts in the hard X-ray band \citep{zdz94,mad95,zdz96,brenneman2014a}.

NGC~985 is a southern Seyfert~1 galaxy at $z=0.0427$ \citep{Fisher1995} whose black hole mass is $\sim2.2\times10^8~M_\odot$ \citep{kim2008}. NGC~985 is a peculiar galaxy with a prominent ring-shaped zone at several kiloparsecs from the nucleus \citep{deVaucouleurs1975}, suggesting that the galaxy is under- going a merging process. The galaxy contains a double nucleus, Seyfert nucleus, and non-AGN \citep{PerezGarcia1996}. The nuclei are separated by 3~arcsec.

\subsection{Radio observations with ALMA}
We observed IC~4329A and NGC~985 on October 2nd, 2016 and August 18th, 2017, respectively, using the ALMA Band~3, ~4, and 6 receivers (project-ID:  $\#$2016.1.01140.S, PI = Y. Inoue).

For the IC~4329A observation, J1427-4206 and J1351-2912 were observed as a flux calibrator and phase calibrator, respectively.  Additionally, J1349-3056 was also observed for Band~6 as a water vapor radiometer calibrator.
For the NGC~985 observation, J0238+1636 and J0241-0815 were observed as a flux calibrator and phase calibrator, respectively, for Bands 3 and 4, while J0334-4008 and J0241-0815 were observed as a flux calibrator and phase calibrator, respectively, for Band 6. Additionally, J0243-0550 was also observed as a water vapor radiometer calibrator.

Four spectral windows (SPWs) with a bandwidth of 2.000~GHz were placed at sky frequencies centered at 90.5~GHz, 92.4~GHz, 102.5~GHz, and 104.5~GHz in Band~3, at 138.0~GHz, 139.9~GHz, 150.0~GHz, and 152.0~GHz in Band~4, and at 213.0~GHz, 215.0~GHz, 229.0~GHz, and 231.0~GHz in Band~6. The correlation was made in the Time Division Mode with 128~channels for an SPW.

The data were calibrated using the ALMA reduction package {\tt CASA} version 4.7.0 \citep{McMullin:2007}.  We reduced raw data using pipeline scripts provided by the ALMA regional center.

For IC~4329A observation, the flux scaling factors were determined with reference to the quasar J1427-4206 at all bands.  For NGC~985 observations, the flux scaling factors were determined with reference to the quasar J0238+1636 at Bands 3 and 4, and J0334-4008 at Band~6.
Their flux densities are regularly monitored by the ALMA observatory. We queried the ALMA calibrator database to make the assurance doubly sure.  J1427-4206 was stable ($\sim2.5~{\rm Jy}$ and $\sim1.2~{\rm Jy}$ at Bands~3 and 6, respectively) during the period before and after the dates of ALMA observations. The flux scaling factors used in the pipelines were based on a power-law spectrum that was determined from Band-3/7 observations carried out by the observatory within 7~days of our ALMA observations.  The flux densities of J0238+1636 and J0334-4008 were determined from Band-3/7 observations carried out by the observatory 2~days before our ALMA observations.

We confirmed that no line emission practically contributes to the observed frequency ranges. Although a possible absorption feature by the Earth's atmosphere is seen at $\sim231.5~{\rm GHz}$ (spw~3 in Band~6), this does not affect the photometry of continuum emission.

The calibrated visibilities were exported for four individual SPWs, and processed for mapping and CLEANing using natural weighting. Consequently, we obtained four continuum images for each band. The images were analyzed with the {\tt CASA}.  The ratio between peak flux density and integrated flux density was $\sim93$\%, $\sim92$\%, and $\sim85$\% for Band~3, 4, and 6, respectively, in the case of IC~4329A, while it was $\sim96$\%, $\sim90$\%, and $\sim90$\% in the case of NGC~985. Thus, unresolved sources dominate the emission in all the images.

The emission center of the IC~4329A nucleus is located at $\alpha=$ 13h49m19.26170s $\pm 0.00262^{\prime\prime}$,   $\delta = -30^\circ$18$^\prime$34.22145$^{\prime\prime}\pm0.00264^{\prime\prime}$ (J2000) at 150~GHz.
The emission center of the NGC~985 nucleus is located at  $\alpha=$ 02h34m37.84028s $\pm 0.00244^{\prime\prime}$, $\delta = -08^\circ$47$^\prime$16.07808$^{\prime\prime}\pm0.00173^{\prime\prime}$ (J2000) at 150~GHz.
These are the best determined positions ever for these Seyfert nuclei where a systematic error is included. An astrometric position error on the phase calibrator was determined to be in a sub-milli-arcsecond level in the 2nd International Celestial Reference Frame \citep{Ma2009}.

The flux measurements were performed by a Gaussian fit using the {\tt CASA} task {\tt IMFIT}. Results are summarized in Tables.~\ref{table:observation_ic4329a} and \ref{table:observation_ngc985}. We assume that the accuracy of the absolute amplitude calibration is 5\% for Bands 3 and 4, and 10\% for Band 6 following the ALMA Proposer's Guide. No other emission was found in a field of view of  $\sim 10~{\rm arcsec}$, even on higher signal-to-noise images that we made from visibilities concatenated throughout the four SPWs.

\begin{table*}
\caption{Spectral analysis results of ALMA, VLA, and ATCA observations of IC~4329A.\label{table:observation_ic4329a}}
\begin{center}
\begin{footnotesize}
\begin{tabular}{ccccccccc}
\hline
\hline
$\nu$   &   $F_\nu$         &   $\sigma$   &   $\theta_\mathrm{maj} \times \theta_\mathrm{min}$         &   $PA$  & Date \\
(GHz)   &   (mJy)         &   (mJy/beam)   &   (arcsec$\times$arcsec)         &   (deg)   & (yr-m-d) \\
(1)   &   (2)   &   (3)         &   (4)   &   (5) & (6)\\
\hline
\multicolumn{6}{c}{ALMA}\\
\hline
90.5 & $8.00\pm0.49$ &  $0.094$ & $0.45  \times 0.44$  & $-25.3$ & 2016-10-02\\
92.4 & $7.92\pm0.49$  & $0.096$ & $0.44  \times 0.43$  & 24.6 & 2016-10-02 \\
102.5 & $8.07 \pm0.50 $  & $0.11$  & $0.43  \times 0.40$  & 20.0 & 2016-10-02 \\
104.5 & $7.81 \pm0.47 $  & $0.10$  & $0.42  \times 0.39$  & 23.7 & 2016-10-02 \\
138.0 & $6.69 \pm0.38 $  & $0.097$  & $0.28  \times 0.25$  & $-173.2$ & 2016-10-02 \\
139.9 & $6.79 \pm0.39 $  & $0.11$  & $0.27  \times 0.25$  & 18.9 & 2016-10-02 \\
150.0 & $6.45 \pm0.39 $  & $0.10$  & $0.29  \times 0.24$  & 26.0 & 2016-10-02 \\
152.0 & $6.27 \pm0.38 $  & $0.13$  & $0.25  \times 0.23$  & 9.6 & 2016-10-02\\
213.0 & $4.39 \pm1.21 $  & $0.16$  & $0.17  \times 0.15$  & 21.8 & 2016-10-02 \\
215.0 & $4.85 \pm0.84 $  & $0.15$ & $0.18  \times 0.16$  & 62.6 & 2016-10-02 \\
229.0 & $5.17 \pm0.92 $  & $0.15$  & $0.18  \times 0.14$  & 34.9 & 2016-10-02 \\
231.0 & $4.98 \pm0.94 $  & $0.16$ & $0.16  \times 0.14$  & 19.5 & 2016-10-02  \\
\hline
\multicolumn{6}{c}{VLA}\\
\hline
1.4	&$	66.8	\pm	4.7	$&$	2.10	$&$	45.0	\times	45.0	$&$	0.0	$&	1995-01-18	\\
1.4	&$	60.5	\pm	2.4	$&$	0.77	$&$	8.1	\times	3.6	$&$	48.1	$&	1998-02-08	\\
1.5	&$	63.5	\pm	4.8	$&$	2.20	$&$	45.0	\times	45.0	$&$	0.0	$&	1991-03-08	\\
4.9	&$	33.1	\pm	1.4	$&$	0.49	$&$	35.2	\times	10.1	$&$	11.6	$&	1991-03-08	\\
4.9	&$	19.5	\pm	0.8	$&$	0.25	$&$	1.3	\times	0.5	$&$	17.6	$&	1986-04-03	\\
8.4	&$	13.9	\pm	1.2	$&$	0.59	$&$	0.8	\times	0.4	$&$	-26.2	$&	1995-07-15	\\
8.4	&$	15.5	\pm	0.7	$&$	0.23	$&$	4.1	\times	1.8	$&$	-48.0	$&	1998-02-08	\\
\hline
\multicolumn{6}{c}{ATCA}\\
\hline
4.8	&$	28.5 	\pm	1.6 	$&$	0.65 	$&$	7.2	\times	2.5	$&$	9.6	$&	2008-04-19	\\
5.5	&$	34.6 	\pm	1.2 	$&$	0.31 	$&$	48.1	\times	30.6	$&$	69.3	$&	2010-03-04	\\
8.6	&$	17.8 	\pm	1.6 	$&$	0.77 	$&$	3.9	\times	1.4	$&$	9.6	$&	2008-04-19	\\
9.0	&$	24.4 	\pm	1.2 	$&$	0.45 	$&$	29.0	\times	18.5	$&$	69.3	$&	2010-03-04	\\
33.0	&$	14.3 	\pm	1.6 	$&$	0.32 	$&$	8.5	\times	5.0	$&$	-86.1	$&	2009-04-25	\\
35.0	&$	14.7 	\pm	1.7 	$&$	0.41 	$&$	8.0	\times	4.7	$&$	-86.1	$&	2009-04-25	\\
\hline
\end{tabular}
\end{footnotesize}
\end{center}
\begin{flushleft}
\begin{footnotesize}
Col.~(1) center frequency;
Col.~(2) total flux density;
Col.~(3) image r.m.s.~noise in the blank sky;
Col.~(4)--(5) synthesized beam sizes along the major axis, minor axis, and position angle of the major axis, respectively;
Col.~(6) observation date.
\end{footnotesize}
\end{flushleft}
\end{table*}

\begin{table*}
\caption{Spectral analysis results of ALMA, VLA, and ATCA observations of NGC~985.\label{table:observation_ngc985}}
\begin{center}
\begin{footnotesize}
\begin{tabular}{ccccccccc}
\hline
\hline
$\nu$   &   $F_\nu$         &   $\sigma$   &   $\theta_\mathrm{maj} \times \theta_\mathrm{min}$         &   $PA$  & Date \\
(GHz)   &   (mJy)         &   (mJy/beam)   &   (arcsec$\times$arcsec)         &   (deg)   & (yr-m-d) \\
(1)   &   (2)   &   (3)         &   (4)   &   (5) & (6)\\
\hline
\multicolumn{6}{c}{ALMA}\\
\hline
90.5	& $	1.72 	\pm	0.12 	$ & 	$0.058$ 	& $	0.25	\times	0.22	$ & $	87.7	$ &	2017-08-18	\\
92.4	& $	1.92 	\pm	0.13 	$ & 	$0.050$ 	& $	0.25	\times	0.21	$ & $	98.9	$ &	2017-08-18	\\
102.5	& $	1.64 	\pm	0.13 	$ & 	$0.059$ 	& $	0.23	\times	0.19	$ & $	84.7	$ &	2017-08-18	\\
104.5	& $	1.59 	\pm	0.13 	$ & 	$0.067$ 	& $	0.22	\times	0.19	$ & $	101.2	$ &	2017-08-18	\\
138.0	& $	1.71 	\pm	0.14 	$ & 	$0.058$ 	& $	0.17	\times	0.14	$ & $	100.0	$ &	2017-08-18	\\
139.9	& $	1.54 	\pm	0.12 	$ & 	$0.048$ 	& $	0.18	\times	0.15	$ & $	83.2	$ &	2017-08-18	\\
150.0	& $	1.44 	\pm	0.12 	$ & 	$0.052$ 	& $	0.16	\times	0.13	$ & $	99.0	$ &	2017-08-18	\\
151.8	& $	1.57 	\pm	0.12 	$ & 	$0.058$ 	& $	0.16	\times	0.13	$ & $	100.3	$ &	2017-08-18	\\
213.0	& $	1.35 	\pm	0.10 	$ & 	$0.041$ 	& $	0.12	\times	0.10	$ & $	84.4	$ &	2017-08-18	\\
215.0	& $	1.27 	\pm	0.10 	$ & 	$0.044$ 	& $	0.12	\times	0.09	$ & $	83.2	$ &	2017-08-18	\\
229.2	& $	1.26 	\pm	0.10 	$ & 	$0.040$ 	& $	0.11	\times	0.09	$ & $	85.6	$ &	2017-08-18	\\
231.0	& $	1.22 	\pm	0.09 	$ & 	$0.037$ 	& $	0.11	\times	0.09	$ & $	86.4	$ &	2017-08-18	\\
\hline
\multicolumn{6}{c}{VLA}\\
\hline
1.4	& $	13.1	\pm	1.0	$ & 	$0.45$	& $	45.0	\times	45.0	$ & $	0.0	$ &	1982-05-30	\\
4.9	& $	1.2	\pm	0.3	$ & 	$0.10$	& $	0.5	\times	0.4	$ & $	-18.7	$ &	1982-05-30	\\
14.9	& $	1.8	\pm	0.8	$ & 	$0.40$	& $	2.2	\times	1.5	$ & $	-14.9	$ &	1985-07-28	\\
1.5	& $	13.0	\pm	1.0	$ & 	$0.58$	& $	26.3	\times	15.3	$ & $	-33.1	$ &	1986-11-08	\\
4.9	& $	3.7	\pm	0.2	$ & 	$0.10$	& $	8.0	\times	4.6	$ & $	-31.1	$ &	1986-11-08	\\
1.5	& $	4.0	\pm	1.6	$ & 	$0.80$	& $	4.8	\times	2.8	$ & $	19.7	$ &	1990-05-23	\\
4.9	& $	1.6	\pm	0.7	$ & 	$0.24$	& $	1.4	\times	0.9	$ & $	10.3	$ &	1990-05-23	\\
8.4	& $	1.1	\pm	0.2	$ & 	$0.12$	& $	0.9	\times	0.7	$ & $	78.5	$ &	1990-05-23	\\
22.5	& $	1.9	\pm	0.3	$ & 	$1.68$	& $	3.8	\times	1.7	$ & $	72.3	$ &	2001-09-28	\\
8.5	& $	0.8	\pm	0.1	$ & 	$0.04$	& $	0.4	\times	0.2	$ & $	12.0	$ &	2003-06-19	\\
8.5	& $	1.3	\pm	0.1	$ & 	$0.10$	& $	1.7	\times	0.8	$ & $	-41.2	$ &	2003-12-24	\\
14.9	& $	0.8	\pm	0.3	$ & 	$0.25$	& $	0.9	\times	0.4	$ & $	-39.3	$ &	2003-12-24	\\
22.5	& $	1.2	\pm	0.3	$ & 	$0.13$	& $	0.5	\times	0.3	$ & $	-35.2	$ &	2003-12-24	\\
43.3	& $	3.1	\pm	1.2	$ & 	$0.62$	& $	0.3	\times	0.1	$ & $	-30.2	$ &	2003-12-24	\\
\hline
\multicolumn{6}{c}{ATCA}\\
\hline
19.0	& $	1.7 	\pm	0.7 	$ & 	$0.39$ 	& $	16.1	\times	8.6	$ & $	57.2	$ &	2009-10-15	\\
19.0	& $	1.7 	\pm	0.6 	$ & 	$0.38$ 	& $	17.7	\times	9.2	$ & $	-72.7	$ &	2009-10-16	\\
19.0	& $	2.0 	\pm	0.7 	$ & 	$0.39$ 	& $	15.8	\times	8.7	$ & $	57.3	$ &	2009-10-17	\\
21.0	& $	4.9 	\pm	1.9 	$ & 	$0.55$ 	& $	14.6	\times	7.8	$ & $	57.2	$ &	2009-10-15	\\
21.0	& $	2.3 	\pm	0.9 	$ & 	$0.22$ 	& $	16.0	\times	8.3	$ & $	-72.7	$ &	2009-10-16	\\
21.0	& $	1.5 	\pm	0.7 	$ & 	$0.39$ 	& $	14.3	\times	7.8	$ & $	57.3	$ &	2009-10-17	\\
\hline
\end{tabular}
\end{footnotesize}
\end{center}
\begin{flushleft}
\begin{footnotesize}
Same as in Table. \ref{table:observation_ic4329a}.
\end{footnotesize}
\end{flushleft}
\end{table*}

\subsection{Low-frequency radio data from VLA and ATCA observations}
We retrieved archival data obtained using the VLA and the ATCA from the US National Radio Astronomy Observatory and the Australia Telescope National Facility, respectively, to examine low-frequency components associated with the Seyfert nuclei.  For IC~4329A we retrieved all available data from the data archive centers; the observation codes were AE76, AM384, AS230, and AK394 for the VLA data and C1803 and C1964 for the ATCA data.  For NGC~985, we retrieved archival data with codes AB417 and AB489 for the VLA data and C1964 for the the ATCA data.  Additionally, we used the results of previous VLA studies for NGC~985 \citep{doi2016}.  We also retrieved and analyzed the 1.4-GHz images from the NRAO VLA Sky Survey~(NVSS; \citep{Condon:1998}).

The VLA data were reduced in the standard manners for continuum observations using the software Astronomical Image Processing System~\citep[{\tt AIPS};][]{Greisen:2003}. Calibrations were carried out in accordance with the guidelines for the accurate flux density bootstrapping. Flux density bootstrapping covers the corrections for the elevation dependences of the gain curve for antenna elements and of atmospheric opacity. It also covers self-calibration procedures with the source structure models for standard flux calibrators and with a point source model for gain calibrators.

The accuracy of flux scaling is 1\%--2\% at 8.4~GHz or lower in VLA observations; we assume a 3\% error in the present study, conservatively.  All target images were generated from calibrated visibilities with natural weighting in addition to deconvolution through the CLEAN algorithm. A single emission component was clearly detected at the position of the nucleus.  The source identification was performed by Gaussian model fitting on each image using the {\tt AIPS} task {\tt JMFIT}.  The final error of the flux density measurements was determined by root-sum-squares of the Gaussian fitting error and the flux scaling uncertainty. The fitting results were indicative of an underlying emission that was slightly resolved to be a few~arcsec in diameter on images with a compact array configuration.  In NGC 985, it is known that a radio emitting region of star formation was located $\sim17\arcsec$ westward from the nucleus \citep{Appleton2002}.  The NVSS image actually shows a westward elongation.  We made image-based model fitting with two components and subtracted the contribution of the western component from the total flux densities for the NVSS and the AB417 at 1.5~GHz.

The ATCA data were also reduced in the standard manners using the software {\tt Miriad} \citep{Sault:1995}.  The ATCA observation and data analysis procedure also follows a philosophy that is very similar to the VLA observation. Corrections to atmospheric opacity, antenna positions, and system temperature measurements were applied to the data obtained at 19~GHz or higher frequencies.  We assume flux scaling errors of 10\% and 3\% at 33/35~GHz and other lower frequencies, respectively, according to the ATCA user guide.  Target images were synthesized with natural weighting and the CLEAN deconvolution.  Flux density measurements were carried out in the same manner as in the VLA data analysis, using the {\tt AIPS} task {\tt JMFIT}.  The VLA and ATCA results are listed in Tables~\ref{table:observation_ic4329a} and \ref{table:observation_ngc985}.

\subsection{X-ray data analysis of NGC~985}
\label{app:xray}
For the thermal coronal properties of IC~4329A, we adopted the data analysis results of the joint {\it Suzaku} and {\it NuSTAR} observations toward IC~4329A  \citep{brenneman2014b}. They found that the coronal temperature and the Thomson scattering optical depth are 50~keV and 2.34, respectively, assuming a spherical geometry. For NGC~985, we analyze archival {\it NuSTAR} data in order to derive coronal properties. Coronal parameters are determined by characteristics of primary high-energy continuum. Therefore, we restrict our analysis to 5--79~keV in order to avoid the effects of low-energy absorption, which are poorly constrained by {\it NuSTAR} only.

\begin{figure}
 \begin{center}
  \includegraphics[width=7.5cm]{xray_spctr_NGC985.pdf}
 \end{center}
\caption{Upper panel: The {\tt compTT} + {\tt pexmon}  spectral model fit in the range of 5--79~keV to the FPMA (black) and FPMB (red) data. Lower panel: data-to-model ratio for the FPMA (black) and FPMB (red). The horizontal line shows a ratio of unity for reference.
}\label{fig:xray_ngc985}
\end{figure}

{\it NuSTAR} is a focusing hard X-ray telescope providing a bandpass of 3--79~keV with a spectral resolution of $\sim1$~keV \citep{har13}. {\it NuSTAR} observed NGC~985 on August 11, 2013 (obsid: 60061025002). After eliminating Earth occultations, passages through the South Atlantic Anomaly, and other periods of high background, the NuSTAR observation reached $\sim13.9$ ks of on-source time for focal plane module A (FPMA) and focal plane module B (FPMB).

We reduced the data using the NuSTAR Data Analysis Software (NuSTARDAS) and calibration version 1.4.1. We filtered the event files and applied the default depth correction using the nupipeline task. We used circular extraction regions, 45 arcsec in radius, for the source and background, with the source region centered on NGC~985 and the background taken from the corner of the same detector, as close as possible to the source without being contaminated by the point spread function wings. Spectra and images were extracted and response files were generated using the nuproducts task. To minimize systematic effects, we fitted spectra from FPMA and FPMB simultaneously. We allowed the absolute normalization for both modules to vary. We found a cross-calibration factor of $1.05^{+0.45}_{-0.23}$ for FPMB relative to FPMA.

Given the short exposure, we followed the analysis procedure of IC~4329A \citep{brenneman2014a}. we first evaluated the {\it NuSTAR} spectrum with the {\tt pexmon} model \citep{Nandra2007}, which incorporates both primary emission and reflection. We fixed the abundance of elements to the solar abundances, the inclination angle of $i=60^\circ$, otherwise we cannot get any constraints on other parameters. The foreground Galactic column density was set to $N_{\rm H} = 3.17\times 10^{20}$~${\rm cm^{-2}}$ \citep{Kalberla2005}. We got $\Gamma=1.71\pm0.08$, $E_{\rm cut}=99_{-27}^{+19}~{\rm keV}$, and $R=0.80_{-0.14}^{+0.31}$ with a goodness-of-fit of $\chi^2/\nu=191/145 (1.32)$.

Then, to derive physical parameter of the corona, we employed the {\tt compTT} model \citep{Titarchuk1994}, which calculates the Comptonization spectra. {\tt compTT} does not self-consistently calculate the reflection component. Thus, we added the reflection component by using {\tt pexmon}.  We set the cutoff energy in {\tt pexmon} to 2.7 times of the coronal electron temperature. We fixed the other values of the reflection component to the values found for the {\tt pexmon} fit and include only the reflection part of the model. We found the coronal temperature of $kT_e=29_{-9}^{+5}~{\rm keV}$ and the Thomson scattering optical depth of $\tau=3.5_{-0.6}^{+1.2}$ with a goodness-of-fit of $\chi^2/\nu=191/146 (1.31)$. In order to obtain the better fit, we may need further exposure. The resulting spectrum is shown in Figure. \ref{fig:xray_ngc985}.

\begin{figure}
 \begin{center}
  \includegraphics[width=7.5cm]{Calibrator_all.pdf}
 \end{center}
\caption{The mm spectra of J1427-4206 (Flux calibrator, triangle), J1351-2912 (Phase calibrator, square), and IC~4329A (Target, circle) taken by ALMA. Each data point shows its 1-$\sigma$ error bar. Data points of J1427-4206 and J1351-2912 are renormalized by a factor of 0.006 and 0.03, respectively. The solid and dashed lines correspond to the single power-law fit to J1428-4206 and J1351-2912, respectively.}\label{fig:calibrator}
\end{figure}

\begin{figure*}
 \begin{center}
  \includegraphics[width=8.9cm]{SED_IC4329A_data.pdf}
  \includegraphics[width=8.9cm]{SED_NGC985_data.pdf}
 \end{center}
\caption{{\it Left}: The cm-mm spectrum data of IC~4329A. The magenta, blue, and green points show the VLA, ATCA, and ALMA data, respectively. The error bars correspond to 1-$\sigma$ uncertainties. A circle around each data point represents the scaled synthesized beam size. The beam size dependency is presented as circles in the panel for the cases of $10\arcsec$, $1\arcsec$, and $0\farcs1$.  {\it Right}: Same as the left panel but for NGC~985.  The ATCA measurements at 19 and 21~GHz were averaged throughout three consecutive days.}\label{fig:SED_radio_raw}
\end{figure*}

\section{Results}
\label{sec:result}
Figure.~\ref{fig:calibrator} shows the mm spectrum of our target object IC~4329A together with those of the flux calibrator J1427-4206 and the phase calibrator J1351-2912. The flux of J1427-4206 and J1351-2912 in Figure.~\ref{fig:calibrator} is renormalized by a factor of 0.006 and 0.03, respectively, for the comparison with the target object IC~4329A. The spectra of J1427-4206 and J1351-2912 are well reproduced by single power-law models, while our target object IC~4329A shows spectral curvature (Figure. \ref{fig:calibrator}). We do not see such curvature features in the ALMA data of NGC~985.

The left and right panel of Figure. \ref{fig:SED_radio_raw} shows the observed cm-mm radio spectral data of IC~4329A and NGC~985, respectively. Different beam size data are included ranging from 0.15" to  45.0" for IC~4329A and from 0.10" to  45.0" for NGC~985 (Tables~\ref{table:observation_ic4329a} and \ref{table:observation_ngc985}). Geometric mean of synthesized beam sizes at major and minor axes for each data is also represented in the Figure. In both objects, a clear tendency of higher flux densities at larger beam sizes is apparent. For large beam size data sets, it is naturally expected that extended emission such as host galaxy component contributes to photometry, while such extended emission does not significantly contribute to small beam size data sets. Therefore, consideration of observational beam size is important for the understanding the emission from the compact regions.

\begin{figure*}
 \begin{center}
  \includegraphics[width=8.9cm]{SED_IC4329A_paper.pdf}
  \includegraphics[width=8.9cm]{SED_NGC985_paper.pdf}
 \end{center}
\caption{{\it Left}: The cm-mm spectrum of IC~4329A after subtracting extended emission due to galactic star formation activity. The square, circle, and triangle points show the VLA, ATCA, and ALMA data, respectively. The error bars correspond to 1-$\sigma$ uncertainties where we take into account flux measurement uncertainties and galactic component model uncertainties. The dashed and dotted lines show the fitted hybrid corona and jet component, respectively, with parameters shown in Table.~\ref{table:spectral_data}. The solid line shows the sum of these two components. {\it Right}: Same as the left panel but for NGC~985.  The ATCA measurements at 19 and 21~GHz were averaged throughout three consecutive days.}\label{fig:SED_radio}
\end{figure*}

In order to investigate the origin of the radio emission, we simultaneously fit ALMA, VLA, and ATCA measurements between 1~GHz and 250~GHz with four spectral components. One is synchrotron emission from a hybrid corona \citep{inoue2014} in which fitting parameters are the plasma size ($R$), the magnetic field strength ($B$), the spectral index of non-thermal electrons ($p$), and  the energy fraction of non-thermal electrons ($\eta$). The coronal temperature and the Thomson scattering optical depth are determined by X-ray spectral analysis  \citep[e.g.,][]{brenneman2014b}. We adopt spherical geometry for coronae for simplicity. We define the distribution of electrons in hybrid coronae as relativistic Maxwellian distribution at $\gamma_e \le \gamma_{\rm br}$ and $n_e(\gamma_e)\propto({\gamma_e}/{\gamma_{\rm br}})^{-p} $ at $ (\gamma_e > \gamma_{\rm br})$, where $\gamma_e$ is the electron Lorentz factor and $\gamma_{\rm br}$ is the break Lorentz factor. By setting $\eta$, $\gamma_{\rm br}$ can be obtained. Second is a jet synchrotron emission component represented by the form $F(\nu)=A_{\rm Jet}(\nu/\nu_0)^{\alpha_{\rm Jet}}$ setting $\nu_0=100~{\rm GHz}$. The other two components represent galactic thermal bremsstrahlung and galactic synchrotron of the form $F(\nu, \theta_{\rm maj}, \theta_{\rm min})=A_{\rm SF, FF}(\nu/\nu_0)^{-0.1} \allowbreak \min(1.0, \theta_{\rm maj}\theta_{\rm min}/\theta_{\rm SF}^2)$ and $A_{\rm SF, Syn}\allowbreak(\nu/\nu_0)^{-0.8}\allowbreak\min(1.0, \theta_{\rm maj}\theta_{\rm min}/\theta_{\rm SF}^2)$, where $\theta_{\rm maj}$ is the beam size along the major axis, $\theta_{\rm min}$ is that along the minor axis, and $\theta_{\rm SF}$ gives the angular size of the star formation activity region around the Seyfert nuclei. We set a spectral index of $0.1$ for the thermal free-free component and the spectral index of $0.8$ for the galactic synchrotron component \citep{Magnelli2015}. Since the angular resolutions of observations by VLA and ATCA were not as good as that of ALMA (Figure. \ref{fig:SED_radio_raw}), the measured fluxes by VLA and ATCA must have been contaminated not only by the jet but also by extended emission due to star formation activity in the host galaxy. Therefore, we consider beam sizes and $\theta_{\rm SF}$ in our modeling.

The left panel of Figure. \ref{fig:SED_radio} shows the cm-mm radio spectrum of IC~4329A after we subtract beam-size dependent extended galactic emission components. The mm excess is clearly visible in the cm--mm spectrum, which determines the properties of the coronae. The measured ALMA spectrum of IC~4329A exhibits flattening below 100~GHz, while calibrators' spectra exhibit simple power-law shape (Figure. \ref{fig:calibrator}). This indicates SSA in a very compact region in the order of several tens of the Schwarzschild radius. The measured spectra are well reproduced by the assumed models without time variability.

The coronal properties of IC~4329A are estimated as $R=39\pm10~r_s$ with $B=9\pm6$~G and $p=2.9\pm0.9$ based on our model fitting. The coronal temperature and the Thomson scattering optical depth are set to 50~keV and 2.34, respectively \citep{brenneman2014b}. We fix the energy fraction $\eta$ of non-thermal electrons as 4\% of that of the total electron population. This value is inferred from the explanation of the cosmic MeV gamma-ray background radiation by Seyferts \citep{Inoue2008}. Because $\eta$, $B$, and $R$ are closely tied \citep{inoue2014}, current radio data do not allow us to solve these three parameters simultaneously without decoupling thermal and non-thermal components. Future simultaneous radio and sub-MeV gamma-ray observations will enable us to estimate more precise model parameters. Even if we vary $\eta$ from 0.01 to 0.30, the parameters $B$, $R$, and $p$ are consistent within an uncertainty of 1-$\sigma$. Current X-ray observations of Seyferts constrain $\eta<0.3$ \citep{fabian2017}.

The right panel of Figure. \ref{fig:SED_radio} shows the cm-mm radio spectrum of NGC~985 after subtracting extended galactic components, same as in IC~4329A. Again, the mm excess is clearly seen. We fit the spectrum with the same models for IC~4329A. For the X-ray coronal properties, we adopt the coronal temperature and the optical depth due to Thomson scattering of 29~keV and 3.5, respectively (see Section. \ref{app:xray}). The coronal properties of NGC~985 are estimated as $(R, B, p) = (47\pm21~r_s, 4\pm2~{\rm G}, 2.1\pm0.3)$, setting $\eta=0.04$. The obtained parameters for both systems are summarized in Table. \ref{table:spectral_data}.

\begin{table}
\caption{Spectral fitting results in the frequency range of 1~GHz to 250~GHz.\label{table:spectral_data}}
\begin{center}
\begin{footnotesize}
\begin{tabular}{crr}
\hline
\hline
Parameter & IC~4329A & NGC~985 \\
\hline
\multicolumn{3}{c}{Hybrid corona}\\
\hline
$p$ & $2.90\pm0.86$ & $2.11\pm0.28$\\
$B$ (G) & $9.42\pm6.16$ & $4.18\pm 1.90$\\
$R$ ($r_s$) & $38.8\pm9.7$	 & $46.9\pm20.5$	\\
$\eta$ & $0.04$ (fixed) & $0.04$ (fixed)\\
\hline
\multicolumn{3}{c}{Jet}\\
\hline
$A_{\rm Jet}$ (mJy) & $3.23\pm0.79$ & $0.61\pm0.20$\\
$\alpha_{\rm Jet}$& $-0.59\pm0.09$& $-0.18\pm0.13$\\
\hline
\multicolumn{3}{c}{Star formation activity}\\
\hline
$A_{\rm SF, Syn}$ (mJy) & $0.60\pm0.28$ & $0.38\pm0.03$\\
$A_{\rm SF, FF}$ (mJy) & $6.16\pm1.92$ & $<0.35$\\
$\theta_{\rm SF}$ (arcsec)& $6.05\pm0.39$ & $7.69\pm0.47$\\
\hline
$\chi^2/{\rm d.o.f}$ & $11.3/17$ & $22.5/20$\\
\hline
\end{tabular}
\end{footnotesize}
\end{center}
\begin{flushleft}
\begin{footnotesize}
The errors and the upper limit correspond to 1-$\sigma$ uncertainties. The upper limit is the 1-$\sigma$ upper limit.
\end{footnotesize}
\end{flushleft}
\end{table}

\section{Discussion}
\label{sec:dis}

\subsection{Variability}
Both IC~4329A and NGC~985 are known to be relatively steady in X-ray ($\sim50$~\% of flux variability) during  {\it NuSTAR} and ALMA observations \citep{Oh2018,Kawamuro2018}. Such small variabilities will vary $B$ and $R$ for about 10\%, which is smaller than 1-$\sigma$ uncertainties of parameters. Here, compact jets explaining the cm data are also  potentially variable. But, the multi-epoch cm data are consistent with a single power law, indicating no significant variability in the jet components in both Seyferts.

\subsection{Contribution of Other Components}
Thermal dust emission might contribute to the mm flux \citep[e.g.][]{doi2016}. However, given the ALMA spectral shapes, the dust scenario is clearly disfavored because the gray body spectrum from thermal dust shows a much harder spectrum. IC~4329A is known to have a hot nuclear dust component \citep{Mehdipour2018}. The expected compact nuclear dust contamination into the ALMA bands is less than $1.6\times10^{-2}$~mJy.

Would a pure thermal coronal synchrotron emission scenario explain the observed spectra \citep{inoue2014,Raginski:2016}? Considering the X-ray measurements (temperature and Thomson scattering optical depth), the required size for pure thermal coronae become $R\sim2600 r_s$ with $B\sim330$~G for IC~4329A and $R\sim3100 r_s$ with $B\sim180$~G for NGC~985. Such large coronal size is naturally expected for pure thermal synchrotron cases \citep{inoue2014,Raginski:2016}. However, the inferred coronal size are too large comparing to the expected coronal size from other measurements. For example, a combined optical and X-ray study of 51 unobscured AGNs revealed the average corona radii of $(27\pm18)r_s$ \citep{Jin2012}. Microlensing observations toward the Lensed Quasar Q J0158-4325 also inferred the half-light radius for X-ray emission of $\sim10r_s$ \citep{morgan2012}. Given these size constraints, pure thermal electron distribution would be difficult to explain the measured radio spectral data of the two Seyferts.

Here, the SSA peak flux ($\sim10$~mJy) and frequency ($\sim100$~GHz) position are observationally fixed, while the number of high energy electron ($\gamma_e\gg1$) in pure thermal distribution is much less than that in hybrid distribution cases. Thus, the required size and magnetic field strength for thermal models become larger than those in the case of hybrid coronae. We note that the size $R$ and magnetic field $B$ of plasma can also be derived once the SSA frequency and flux are determined. The SSA optical depth is defined as $\tau_{\rm SSA}(\nu)=\alpha_{{\rm Syn}, \nu}R$ where $\alpha_{{\rm Syn}, \nu}$ is the synchrotron absorption coefficient. The SSA frequency $\nu_{\rm SSA}$ is given by $\tau_{\rm SSA}(\nu_{\rm SSA})=1$. The optically thin synchrotron flux is expressed as $F_{\rm Syn}=j_{\rm Syn, \nu} V / 4\pi d^2$ where $j_{\rm Syn, \nu}$ is the synchrotron emissivity, $V=4\pi R^3/3$ is the volume of the plasma, and $d$ is the distance to the object. By adopting synchrotron absorption and emission coefficients \citep{rybicki1979} and setting electron distribution, one can derive $R$ and $B$ by solving above equations.

\subsection{Corona Heating Mechanism and Its Structure}

It is believed that accretion disk coronae are heated by the release of magnetic field energy, like in the Sun, while cooling is dominated by Comptonization by disk photons in the case of disk coronae \citep{haardt91,liu2002}. Based on our measurement, the plasma beta $\beta$ (the ratio of gas pressure to magnetic pressure, $p_{\rm gas}/p_{\rm B}=8\pi nk_BT/B^2$) in the accretion disk coronae becomes $\sim0.1$ for both objects. The inferred plasma beta is higher than that typically observed in the solar corona, $10^{-3}$--$10^{-1}$ \citep{Gary2001}. Given our measurements of two Seyferts, the magnetic heating rate in the coronae is estimated as $Q_{\rm B, heat}\sim10^{10}-10^{11}~{\rm erg~cm^{-2}~s^{-1}}$ (i.e., magnetic energy release rate at the Alfv\'en speed), while the Compton cooling rate by disk photons is $Q_{\rm IC, cool}\sim10^{14}~{\rm erg~cm^{-2}~s^{-1}}$ setting 10\% of the Eddington luminosity. Therefore, magnetic field energy is insufficient for keeping coronae as hot as observed in X-rays.

Here, if the inner part of the accretion disk at several tens of the Schwarzschild radius is composed of a cold disk and a hot accretion flow like an advection-dominated accretion flow \citep[e.g.,][]{yamada2013}, the advection-heated inner accretion region can play the role of coronae \citep{Merloni2000,Kawabata2010}. Observations of a Galactic X-ray binary Cygnus X-1 suggests such an accretion disk picture in order to explain its X-ray spectra and its variability \citep{yamada2013,Basak2017}. In this case, the hot accretion flow would be heated up to electron rest-mass energy \citep{manmoto1997}. Based on the self-similar solutions of hot accretion flows \citep{kato2008,yuan2014}, the magnetic field strength can be estimated as $\sim10$~G at the size of $40r_s$ assuming the $\alpha$ parameter of 0.1 and the mass accretion rate of 0.1\% of the Eddington rate in the inner hot accretion flow. Following the numerical general relativistic magnetohydrodynamic simulations of hot accretion flows, $\beta$ decreases with increasing distance away from the midplane of the disk and becomes $\beta\sim0.1$ above approximately two density scale heights \citep{DeVilliers2003,DeVilliers2005}.  These are consistent with our radio observation results.

Typically, seyferts have much higher accretion rate and the accretion rate  can be determined with reasonable accuracy from the observed optical flux once the black hole mass is known \citep[e.g.,][]{Davis2011}. However, optical emission arises at the outer thin disc region, i.e. the inferred high mass accretion rate is the value at the outer region. The accurate mass accretion rate in the inner region is still not well understood because AGN disk emission peaks in the UV regime which cannot be directly observed due to dust extinction. Moreover, \citet{brenneman2014b} found the equivalent width of the broad iron Fe~K$\alpha$ line emission is 24--42~eV corresponding to the location of cold material at $35 r_s$. This suggests that the optically thick disk may not extend down to the inner region. Therefore, the accretion rate in the inner region could be lower than that measured from optical fluxes.

This cold + hot accretion flow scenario may also present an inconsistency with the general picture of broad iron Fe~K$\alpha$ line emissions originating from near the innermost stable circular orbit and soft X-ray lags  \citep{Reynolds2014,Kara2016}. However, line profiles of Fe~K$\alpha$ lines in Seyferts could be narrower than ever thought, implying the far location of neutral iron, by considering hard X-ray variabilities \citep{Noda2011} or double partial covering materials \citep{Miyakawa2012}. For the IC~4329A, as described above, the location of the origin of the Fe~K$\alpha$ line is found to be at $\sim35r_s$ \citep{brenneman2014b}. The origin of soft X-ray lags is also under debate \citep{Miller2010,Mizumoto2018}.  Future detailed X-ray and radio observations will be important to reconcile these problems.

\subsection{On the Origin of the Cosmic MeV Gamma-ray Background Radiation}
The possible evidence of non-thermal electrons in coronae would shed new light on the origin of the cosmic MeV gamma-ray background, which has been long discussed \citep[see e.g.,][for reviews]{inoue2014_Fermi}. One possible candidate is the MeV non-thermal photon spectral tail expected in Seyfert spectra arisen from non-thermal electrons in coronae \citep[see][for details]{Inoue2008}, while blazars are also considered as a candidate \citep{Ajello2009}. Due to a lack of MeV gamma-ray observations, the origin of the cosmic MeV gamma-ray background is still veiled in mystery, although anisotropy measurements may distinguish these two scenarios \citep{Inoue2013}.

Our radio observations toward nearby Seyferts suggested possible existence of non-thermal electrons in coronae, which is anticipated for the Seyfert scenario on the MeV gamma-ray background. The required non-thermal electron energy fraction for the Seyfert scenario is approximately $4$\% with a spectral index of $\sim3.5$. Future simultaneous radio and MeV gamma-ray observations will be able to quantify amount of non-thermal electrons in coronae and reveal the origin of the MeV background radiation.

\section{Conclusion}
\label{sec:Conclusion}
By utilizing ALMA, we have obtained new measurements for nearby radio-quiet Seyferts IC~4329A and NGC~985 at 12 frequency bands from 90~GHz up to 250~GHz. We further analyzed archival cm data from VLA and ATCA. By combining the mm and cm data sets, the spectra of compact components clearly show the excesses in the mm band.

The measured spectra suggest that the coronal magnetic field is approximately $10$~Gauss on scales of $\sim40r_s$ from the SMBHs for the two Seyferts. This magnetic field strength is weaker than the prediction from the magnetically heated accretion corona scenario \citep[e.g.,][]{liu2002}.  Our mm observation also provides observational evidence of non-thermal electron population in coronae, which may suggest possible contribution of Seyferts to the cosmic MeV gamma-ray background radiation through the Comptonization process of such non-thermal electrons \citep{Inoue2008}.

\acknowledgments
YI is supported by JSPS KAKENHI Grant Number JP16K13813, program of Leading Initiative for Excellent Young Researchers, MEXT, Japan, and RIKEN iTHEMS Program. This paper makes use of the following ALMA data: ADS/JAO. ALMA$\# 2016.1.01140.S$. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This paper also utilizes archival data from VLA operated by NRAO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of archived data obtained through the Australia Telescope Online Archive (\url{http://atoa.atnf.csiro.au}). The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO.

\vspace{5mm}
\facilities{ALMA, ATCA, NuSTAR, VLA}

redpajama_set_name: RedPajamaArXiv


Like sheep, we can realize that we have been so busy nibbling on the grass, our heads to the grindstone of life, that we lift up our heads and awaken to the fact that we are lost and in danger. "We all like sheep have gone astray" is a beautiful movement in Handel's Messiah. So often, we have gone astray in ways that seem harmless or in ways where we can easily rationalize and make excuses. Perhaps this is the most dangerous of ways we become lost.
How Easy It is to Stray!
We do not even recognize it, but we worship a relentless God who in Jesus never gives up offering his radical grace and never stops pursuing lost sheep. "Surely goodness and mercy shall follow me all of my days," says the Psalmist. The Good Shepherd cares so deeply and is so committed to this relationship, that God will not be satisfied until he draws all the world to himself. It is God's desire to find and bring back all the sheep into the sheepfold. People matter to God!
Today, if you are feeling out of sorts or experiencing a sense of confusion and loss of purpose and direction in life; feeling that your heart is yearning for something more, something deeper than what the emptiness of the world has to offer, then hear this message, the Good Shepherd is calling you. The Good Shepherd, Jesus Christ gave His life to rescue you. Stop, sit in the quietness and hear the voice of the Shepherd call your name. He has been seeking you and with relentless grace won't stop until he finds you.
You matter to God. You were not only found, but you were also redeemed and you are dearly loved!
← How to Equip Small Church Leaders?
Beautiful analogy, great post Keith!
Thank you Andy. Have blessed day.
That's a fascinating metaphor. Too true. We are stubborn, and he is patient.
Thank you Brandon thanks for reading and taking time to share your thoughts. Have a great day.


text:
Jars of Clay
Do you ever feel weak? Powerless? Incompetent to do all you're asked to do? Here's the truth: You are! Wait… That doesn't sound like what I'm supposed to say. I'm supposed to say that you're strong and you're talented and that you can do anything you set your mind too. But you can't. And you know it. The Bible tells us the truth: "We have this treasure in jars of clay…" (2 Corinthians 4:7). We are jars of clay. Strong? No. Powerful? No. Weak. Fragile. Sinful. Does that describe you?
There's a reason God wants us to understand how fragile we are. "We have this treasure in jars of clay to show that this all-surpassing power is from God and not from us." When we look at ourselves, we see brokenness and sin. But when we look at Jesus, we see forgiveness and strength. Whatever good there is in us—whatever power lives inside us—all that comes from God, not from us! Paul writes, "We are hard pressed on every side, but not crushed; perplexed, but not in despair; persecuted, but not abandoned; struck down, but not destroyed" (2 Corinthians 4:8-9). What a blessing to carry around God's treasure in our jars of clay!
#2Corinthians #Sin #Strength
Breaking News: God's in Control!
God's Word Isn't Suspended
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text:
FC Dallas, Crew enter stretch run
Sports Xchange
14 Sep 2018, 17:16 GMT+10
FC Dallas and the Columbus Crew SC, two of the most consistent sides in MLS, will try to stay hot when they square off Saturday at Toyota Stadium in Frisco, Texas, for the only time this season as the regular season begins its final stretch.
Both teams come off 12-day layoffs for the late-season international break.
FC Dallas (14-6-7, 49 points) is looking to maintain its lead atop the Western Conference standings. The Huntsmen, who have a one-point lead over Sporting Kansas City, are coming off a 4-2 win over Houston in the Texas Derby on Sept. 1.
Santiago Mosquera tallied a brace in a three-minute span in that victory after Michael Barrios opened the scoring in the 10th minute. Reto Ziegler also scored for FC Dallas, converting from the penalty spot.
"Sometimes with Mosquera, he has all these (abilities) to provide to the team and within the game, and we're trying to capture that," FC Dallas coach Oscar Pareja said of his suddenly-proficent goal-scorer. "Then the injuries obviously break his consistency in the field, so it's not been easy. I'm delighted to see him with such energy and working hard for his teammates."
FC Dallas roars into the stretch run with its focus on two goals: clinch a spot in the playoffs and win the MLS Cup.
"Knowing this group this much and working with them every day, I can see their eagerness to continue the path of getting trophies for the club," Pareja said. "And not being just an important team in the league, but a team who wins it."
Columbus (12-8-7, 43 points) went into the international break on a high note as well, defeating New York City FC 2-1 at home on Sept. 1. The Crew trail third-place NYCFC by six points in the Eastern Conference race and are nine points above the playoff line.
After falling behind in the 53rd minute against NYC, Harrison Afful and Justin Meram scored two minutes apart to produce the win for the Crew.
Columbus has been hot lately, rolling to a 4-1-1 record since July 21. The Crew have five players, including four key starters -- goalkeeper Zack Steffen, Wil Trapp, Gyasi Zardes and Afful -- coming back from international duty for the FC Dallas match.
"Dallas is a very good team," Columbus coach Gregg Berhalter said. "When I look at them throughout the years, it's a very aggressive team, very aggressive on both sides of transition -- offensive transition, defensive transition. They have some good playmakers on their team. We know it's going to be a very difficult game for us."
Columbus defender Jonathan Mensah recognizes the importance of a strong back line heading into the regular-season homestretch.
"We're going to need everyone, so training-wise, we all contribute and improve," Mensah said. "Whoever steps in is going to do the same job, so we just have to be ready whenever you get the opportunity you go out there and help the team."
The Crew own a 19-17 all-time advantage over FC Dallas, with 10 draws. The Huntsmen have won 12 of the 21 matches played in north Texas, with three draws, including the most recent meeting in Frisco, a 1-1 tie in April 2016.


text:
shyshka - Fotolia
Dremio raises $135M to boost data lake transformation effort
The CEO of Dremio outlines why the vendor is growing as organizations increasingly rely on cloud data storage to fuel business intelligence and analytics.
Sean Michael Kerner
Dremio today marked the next major phase of the data lake engine vendor's evolution, raising $135 million in a Series D round of funding.
The challenge of using data lakes effectively is a big opportunity for vendors and enterprises alike.
Dremio, based in Santa Clara, Calif., is among the vendors looking to help organizations enable data lakes to more effectively be used for data intelligence.
The Dremio platform provides a data lake engine that gives organizations the ability to rapidly organize and query information stored in data lakes.
Last year was a busy time for Dremio, appointing new CEO Billy Bosworth in February. Bosworth was previously CEO of database vendor DataStax.
Dremio also released multiple updates to its core platform over the course of the year. In October 2020, Dremio released the Fall 2020 update, with enhancements designed to accelerate cloud data lakes for business intelligence use cases.
In this Q&A, Bosworth details the challenges and opportunities of the data lake market.
Why are you raising money now and was it influenced by the Snowflake IPO (initial public offering)?
Billy Bosworth: When we looked at our operating plans and multiyear projections, we wanted to take a look at a number that would be interesting enough to us to be able to fund very aggressive growth.
Billy Bosworth
This was an opportunistic round of funding as we had just raised $70 million in March 2020. Everything we're focused on right now is purely about scaling the company. We're not looking at any timing for an IPO.
What the Snowflake IPO did was it put an exclamation point on cloud-based analytics. If you really boil it down to what's the biggest trend that Snowflake's success really accentuates, it's that the most important data to be analyzed is very aggressively and rapidly moving into cloud platforms. For that, Dremio offers a solution that really simplifies the data workflow and avoids needless copying of the data and moving of the data into data warehouses.
What has your first year as CEO of Dremio been like during the coronavirus pandemic and how has it been different from your experience leading DataStax?
Bosworth: I joined at the end of February, and I only had two weeks in the office. Then the restrictions started here in Santa Clara and so I've only been in the office with the team physically for a couple of weeks out of the 11 months I've been here.
We went into what I would call very prudent growth operations there for about a three-month period in March, April and May. Then once we saw that people were settling into the new normal during the pandemic, we saw our business start to return to normal as well.
I have been in data and databases and associated with data companies for almost 30 years now. So, for me, living in any form of the data space is a very comfortable position. Growing a company and scaling a company, I do think there are advantages to having done that one once before when it comes to things like fundraising and building an executive team.
Where are the key challenges that organizations face with data lakes today?
Bosworth: This trend emerged from the bottom up, meaning what really started it was the ubiquitous use of the cloud storage layer. It's infinitely scalable and when you look at IT budgets, it's extraordinarily easy to administer, so the data just kept landing there.
Before you know it, you turn around and you see that all of a sudden, the default data bucket for your company has become data lake storage. That was new; normally businesses always thought first about how to get data into a database. Then all of a sudden there it is, all this data in massive quantities waiting to be used.
When we looked at our operating plans and multiyear projections, we wanted to take a look at a number that would be interesting enough to us to be able to fund very aggressive growth.
Billy BosworthCEO, Dremio
The real problem from the top down was -- 'I've got all this data now sitting there that I never planned on actually sitting there and every team in the company is using it, and they're using it increasingly fast, so how do I respond to that? What is the most efficient way to make use of that data going forward?'
That's where people are waking up to the realization that it's a good idea to keep that data in an open format, so that a bunch of other cloud services can use it without having to make additional copies and without moving it all over the place.
That's why Dremio has become interesting for them, because we can help solve that workflow problem of not having to create those additional copies and that additional data movement. That's what's ultimately on their mind. They've got this groundswell of data from the bottom up, a business need to move very quickly and lots of teams that want access to the same data.
Dig Deeper on Database management systems (DBMS)
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Subsurface event reveals what lies below the cloud ... – SearchDataManagement
Dremio Data Lake Engine 4.0 accelerates query ... – SearchDataManagement
Dremio accelerates cloud data lake queries for AWS – SearchDataManagement


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Items tagged with kid
by Shawn Oliver - Wed, Aug 12, 2009
Dell's Nickelodeon Edition Netbook Makes The Kids Go Wild
Anyone paying even the slightest attention to the evolution of Dell designs would know that the company has come a long way since the beige box days in the late 90s, but even for the newer, fresher, hipper Dell, this one's pretty radical. Just as the company decided to dump its Inspiron Mini 12 in favor of keeping just the Mini 10 around, it has decided to tag-team with what's likely the most popular network for kids on television today: Nickelodeon. In a cute, almost slimy joint announcement today, the two are trying to prove that "fun and education can mix" with the Dell Inspiron Mini Nickelodeon Edition, a Mini 10v-based netbook that's obviously designed for kids aged 6 to 106. The giveaway... Read more...
by Daniel A. Begun - Wed, Oct 22, 2008
A Multitouch Table For The Kids
Borrowing from Microsoft's Surface concept, Canadian-based SMART Technologies has designed a multi-touch table designed specifically for the preschool to sixth grade primary educational sector. The SMART Table features a multi-touch-enabled, tabletop 27-inch screen, with an internal projection system and integrated PC. The idea behind the SMART Table is that it gets kids to collaborate with each other while solving problems and playing educational games with an interactive system. "The SMART Table provides a learner-centric experience for small groups that allows students to select or move objects, draw or write on the screen simultaneously, and work together to find answers to preset questions."... Read more...
by Gregory Sullivan - Thu, Aug 14, 2008
Forget Urging Your Kid To Go To Medical School
In the recent past, parents who wanted their children to grow up and make something of themselves would urge them to go to medical or law school. Forget all that. Start urging your children to become independent console game developers. Take Johnathan Blow, for instance. He wrote Braid, a puzzle-solving romp through what looks like hand-painted landscapes, for the Xbox 360. Distribution of games is not reserved just for big players anymore; Johnathon released his creation on Xbox Live Arcade. The result? In its first week, he estimates it's sold about 55,000 copies. Braid has now been out on Xbox Live Arcade for an entire week, and the week has been a good success. The wave of highly-positive... Read more...
by Gregory Sullivan - Mon, May 12, 2008
The DVR Kidnappped Six Million Primetime Viewers
Your Digital Video Recorder might not have found Sarah Conner yet, but it seems to be responsible for the disappearance of six million primetime TV viewers since last May. Some of the miserable ratings of this year's crop of primetime shows could be laid at the feet of the writer's strike, but that really can't explain the whole number. It's starting to dawn on the TV industry that there's no such thing as primetime anymore. ...the more significant shift can't be blamed on the strike. In the past television season, there has been a sharp increase in time-shifting. Some of the six million are still watching, but on their own terms, thanks to TiVos and other digital video recorders, streaming video... Read more...
by Gregory Sullivan - Tue, Oct 02, 2007
Hey, Kids: Rock And Roll -- In Tune This Time
Electronics are supposed to make our lives easier and more pleasant. Gibson guitars have certainly made our lives more pleasant, at least if the proper person is playing them. Gibson decided to make life easier for the guitar player, too, by offering a new line of instruments that tune themselves automatically. Purists say it's cheating, but at least that fellow playing "Stairway To Heaven" at the music store will be playing the wrong notes in tune now.As the strings are played, the Powertune processor compares their actual frequencies with the desired notes and sends instructions--tighten the string this much, loosen the string by that much--to tuning pegs equipped with strong, tiny servo motors... Read more...
by Michael Santo - Fri, Aug 10, 2007
YouTube Launches Missing-Kids Channel
YouTube today launched its "Don't You Forget About Me" channel, which features clips asking for help in finding missing children from around the world. At the time of this writing, the channel has already been viewed over 12,000 times, despite just launching today. YouTube, which was bought by search-engine giant Google (GOOG) last year, began the channel in conjunction with the International Centre for Missing and Exploited Children and the Find Madeleine Campaign, the organization devoted to finding Madeleine McCann, the English toddler who vanished from a hotel in Portugal earlier this summer. You may recall the hit song by Simple Minds, which is the inspiration for... Read more...
by Dave Altavilla - Sun, Apr 29, 2007
New Toys Read Brain Waves, Kids Be Very Afraid
And your kid thought it was hard enough beating that gym boss on Pokemon Diamond. Soon the machine will read their mind too and really start messing with 'em. "A convincing twin of Darth Vader stalks the beige cubicles of a Silicon Valley office, complete with ominous black mask, cape and light saber. But this is no chintzy Halloween costume. It's a prototype, years in the making, of a toy that incorporates brain wave-reading technology. Behind the mask is a sensor that touches the user's forehead and reads the brain's electrical signals, then sends them to a wireless receiver inside the saber, which lights up when the user is concentrating. The player maintains focus by channeling... Read more...
by Gregory Sullivan - Mon, Apr 02, 2007
Hey Kids, Rock And Roll
One of the more unexpected winners in the video game wars is the Guitar Hero franchise. Guitar Hero and Guitar Hero 2 have sold over 3 million copies. EA Games is currently working on taking the franchise to its logical next step and expanding it to four controllers, one each for guitar, bass, drums and vocals. They call it: Rock Band. The songs on the new game haven't been revealed yet. Current games include the Allman Brothers, Joan Jett, Kansas, Nirvana and Wolfmother. "We'll be covering a great breadth, from metal to classic rock to Southern rock to everything in between," Rigopulos says. Online connectivity is a key to the game. The... Read more...


Dr. Wallis is a veteran educator with 27 years of experience. He has served as a superintendent of school for 11 years. He has been named both Texas High School Principal and Superintendent of the year for Texas. Dr. Wallis is a motivational speaker and trainer as well and believes teachers should prepare students for real world experiences - not just state tests. Dr. Wallis has been married to Nicole for 21 years and they are the proud parents of their two boys, Luke and Hunter.
Thank you all for a great two weeks of school! I am proud of each of you and the efforts made getting our students back to normal as quickly as possible after Harvey. In an effort to keep you updated on the happenings around the State and Region, I wanted to report the latest information I received at my last superintendent's meeting.
1. As you are aware, we are two weeks behind districts not affected by Harvey. As of today, we have been told that the state accountability system will not change. Districts and schools will have an accountability rating, as if no disaster had taken place.
2. The Commissioner of Education has stated that he is not opposed to having students who fail the first administration of a given test an opportunity to re-test, but he does NOT think he has the authority to grant this request.
3. Districts in counties declared disasters were given an attendance waiver. The waiver is good through September 8, 2017. Our board adopted the required resolution Monday night and KCISD will not have to make up any days due to Harvey. In addition, the board adopted a resolution granting the district to pay employees for days missed due to Harvey without having to make up those days. Thank you KCISD board.
4. Students who may have enrolled in KCISD, if here during snapshot, will count for our state rating.
5. Due to many of our families affected by Harvey, KCISD will send a Free/Reduced application home to all students next week. Because of the storm, families' financial situations may have changed.
Even though there are variables out of our control, we have control over our thoughts and actions. I am proud of how we have started school and the relationships we have created with families and students in KCISD. Thank you----and as always, remember what is important in life.
Wednesday night, four board members spent over three hours decorating Wildcat Stadium by hanging up banners. We are blessed to have a board that cares enough to roll up their sleeves and do the work.
Not only were board members making Wildcat Stadium shine for our Wildcats, so were three of our Elementary Students. These three helpers were a HUGE help because they secured the bottom portion of the banners (they didn't have as far to bend as we did).
Getting to know these young men was interesting. One of these young men expressed his interest in becoming a biological engineer. WOW, how impressive! To be a 5th grade student and to know his goals already - great stuff. Why is he excited about his future career path? He told me he loves school and his teachers. Thank you KES teachers for making learning fun.
Realizing the HS gym floor has caused a hardship at both the High School and Junior High School, I wanted to report the painting should be finalized this weekend. The painter is working hard to finish as soon a possible. He realizes we want our students at the Junior High back on their court and our Varsity back in the Palace.
Thanks to all volleyball players at both schools for your sacrifices during this unexpected time. We currently have athletes practicing all over the county and on the HS tennis courts. Thank you Gateway Tabernacle for the use of your facility while we are finishing our construction.
Yes I know the title seems like an oxymoron, but I want to take a moment to affirm the KHS band for their uplifting spirits, positive attitudes, and "can do" approach regarding the football game last Friday in Palestine.
Our band, on their way to Palestine, had an unexpected development - the truck transporting their instruments broke down. Arriving at the game with no instruments, no music and no director, they had to improvise when it was time to play our school song. What did they do? Our band, who plays so well, turned into a wonderfully in-tuned choir. Our band sang the school song beautifully. Now, most bands may have just sat down during the game and waited for the instruments to arrive, which they did at half-time, but not our band. They were on their feet, yelling cheers, showing spirit and illustrating un1ty. There are times when we are all proud of our classes, children and family. Friday night was that night for me. Thank you band!
Educational Corner - Having Students Justify their Answers.
Last week we discussed instructing "bell to bell" and not wasting instructional time, due in part to Harvey and our delayed start and the fact that bell-to-bell instruction is a best practice.
This week, let us talk about another teaching tip -- students justifying their answers. This week I have made this more of a research-based section to illustrate the importance of having our students justify their responses.
So how many students should you call on and what types of questions should you ask? According to Hollingsworth and Ybara (2018), they suggest that instructors should consider calling on two students for simple questions and three or more children for more difficult questions. They contend that if these random students called upon are successful, chances are all students are grasping the content taught. However, if the random students are not successful, it is time to reteach.
In their book Explicit Direct Instruction: The Power of the Well-Crafted, Well-Taught Lesson 2nd edition, they penned students should also answer in a loud, public voice that everyone in class could hear. "Try to avoid walking up to individual students to hear a soft voice. When you do this, the other students stop paying attention. Instead, ask students to speak up in a voice you can hear across the room and that all students can hear" (p.56). We know when students are asked to speak in a tone just described; it will begin to build confidence in our children.
Lastly, the authors claim that students should justify all answers -- even simple answers can be higher order when students justify their answers or are asked to provide textual evidence to support their responses. Justifying the answers should be part of your questioning every day.
MathSteps: Grade 1: Justifying Answers: What Is It?