text:
Secretary of State > News > WVSOS Business & Licensing Division to Recognize Businesses and Organizations That Have Been Operating in WV for 100 or More Years
WVSOS Business & Licensing Division to Recognize Businesses and Organizations That Have Been Operating in WV for 100 or More Years
Charleston, W.Va. — There are more than 117,000 entities properly registered to conduct business in West Virginia. Those entities include for-profit corporations as well as charities and non-profit organizations.
The WV Secretary of State's Office is responsible for the proper registration and licensing of each of those business entities. The WVSOS Business & Licensing Division (B&L Division) maintains an updated list of each entity and their classification. Annually this time of the year, every entity is required by state code to file an annual report with the B&L Division.
Each year, about 10,000 new businesses are formed in West Virginia. Some are new companies with dozens or even hundreds of employees. But most are small businesses or sole proprietorships. New businesses are routinely recognized by the media and welcomed to the business community. However, Secretary of State Mac Warner noticed that there isn't a lot of recognition given to those companies and organizations that have stood the test of time and who have been members of the state's business community for a long period of time.
"It is my hope that the WV Centurion Chamber of Commerce will recognize those centurions among our business community, and in a small way, give our state the opportunity to show our appreciation for their leadership and the important role these longstanding businesses have played in maintaining our local and state economies," Secretary Warner said.
The Secretary of State's B&L Division is compiling a list of businesses and organizations in each county that are or will be 100 years old this year. Secretary Warner said that his staff will work with local Chambers of Commerce to host opportunities to recognize these entities before the end of the year.
On Tuesday of this week, Secretary Warner announced the first class of Centurion Chamber members while attending the 100th anniversary dinner of the Harrison County Chamber of Commerce in Clarksburg. Secretary Warner and the Harrison County Chamber board of directors recognized the following Centurions created in or registered in Harrison County:
Clarksburg Country Club, Inc.
Founded on July 10, 1912 in Harrison County, West Virginia
Clarksburg Masonic Building Company, Inc.
Founded August 8, 1907 in Harrison County, West Virginia
Clarksburg Water Board, Inc.
Founded on October 7, 1887
Incorporated on January 28, 1909 in Harrison County, West Virginia
Dominion Energy, Inc.
Originally Founded in 1898 as The Hope Natural Gas Company
In Harrison County, West Virginia
Dyer Insurance Agency, Inc.
Originally Founded as P.M. Long & Son Incorporated
On January 28, 1913 in Harrison County, West Virginia
Harrison County Chamber of Commerce, Inc.
Founded February 5, 1919 in Harrison County, West Virginia
Hartland Planing Mill Company, Inc.
Founded December 24, 1917 in Harrison County, West Virginia
Hornor Brothers Engineers, Inc.
Founded in 1902 in Harrison County, WV
Mon Power – First Energy Corp.
Originally Founded in 1903 as The Fairmont & Clarksburg Traction Company, Inc.
North Central WV Media, Inc.
Originally Founded in 1861 as The Clarksburg Telegram in Harrison County, West Virginia
Northwestern Mutual – Clarksburg District Office
Originally Established by Agent Clyde O. Law in 1913 in Harrison County, West Virginia
Oral Lake Fishing Club, Inc.
Founded April 1, 1914 in Harrison County, West Virginia
R.D. Wilson Sons & Company, Inc.
Founded September 23, 1907 in Harrison County, West Virginia
Rotary Club of Clarksburg, Inc.
Founded July 27, 1916 in Harrison County, West Virginia
Salem University, Inc.
Steptoe & Johnson, PLLC
Founded on 1916 in Harrison County, West Virginia
The Harrison County Bank, Inc.
Founded June 4, 1910 in Harrison County , West Virginia
The James and Law Company, Inc.
Founded March 7, 1903 in Harrison County, West Virginia
The Shinnston News & Harrison County Journal
Originally Founded as The Shinnston News in 1898 in Harrison County, WV
United Hospital Center
The Successor to St. Mary's Hospital, Inc.
Originally Founded on May 13, 1905 in Harrison County, West Virginia
West Virginia Farmers Mutual Insurance Association, Inc.
Founded March 24, 1909 in Harrison County, West Virginia
*Disclaimer: This release is not an endorsement of any business or organization and is intended only for public education purposes.

redpajama_set_name: RedPajamaCommonCrawl


Very soon, for the first time since Prohibition, making your own beer will be legal in all 50 states. On Tuesday, the Alabama Senate passed HB9, legalizing homebrewing in the Cotton State — it was the last to pass such a law. On Thursday, Governor Bentley signed the bill, making it effective immediately.
Dixieland was the last bastion of the ban on brewing at home. Mississippi passed legalization just this March, but, since the law had a 90-day waiting period, it's not quite legal there yet. When the grace period is up, Mississippi will be the last state in the U.S. to allow people to express themselves through suds.
Homebrewing is not that hard, but it's definitely not easy, either. It takes concentration and willingness to be exact and careful with measurements and timing. The results can be fantastic, though, and homebrewers around the world have used their hobby as a jumping off point to launch new craft microbreweries. If you're interested in trying your hand at it, check out the American Homebrewers Association for tips, tricks, recipes and camaraderie, no matter what state you live in.


Standalone: shader with Color Correct map not correctly exported and... red!
I saw some difference between Standalone 2.0 and 4.0 daily.
#1. I have .max file and some shader with the Color Correct map in the DIFFUSE.
#2. Inside the CC I have a simlpe Bitmpa with a wood.jpg.
#3. I want to export the .scn file.
#5. But, in the destination export folder I don't see the wood.jpg!
#6. Strange, because with Corona 2.0, the exported was able to export the wood.jpg.
#7. Now, if I render the .scn files, all the shader originally with the CC map are red!
With Corona 2.0 I was able to render "correctly".
Re: Standalone: shader with Color Correct map not correctly exported and... red!
It's reported in our top secret bug tracker.


How to specify attendees for meal expenses?
Where I live, the accounting laws say that you must specify whether meal expenses are for Representation (i.e. you are hosting external guests for business reasons) or not (i.e. internal employee meals). In our current spreadsheet we must list the attendees and their company name. Is there a way to do this with expensify?
Hi @MikeLong - one of the ways we do this is to put the name etc in the comments section of the expense but we do have some employees that need more room than that and they put all the names in a pdf and attached it to the expense reports referring to the attachment in the expenses comment.
@MikeLong - We are actively researching building out the attendee tracking functionality, but in the meantime @Aussiebandit is correct that the expense comment is the best place for this information.
@Sheena Trepanier any news on attendees?
I don't have an update on attendee tracking right now, but I'll see what I can find out and give you all a heads up once I do.


Yesterday, we told you that Huawei had met the upper end of its target by shipping over 200 million smartphones in 2018. And that accomplishment was achieved despite a very small number of phones delivered to the U.S. market where Huawei is considered a national security threat. The company's P20 series and Mate 20 series both were well received by consumers and industry analysts. One report states that over 16 million units of the former were shipped, half of them to females. Huawei has reportedly shipped 5 million units of the latter series since its October launch. The manufacturer expects to deliver 20 million handsets belonging to the Mate 20 line.
And now, to commemorate the 200 million connected handsets that Huawei delivered this year, the company has announced a special version of its top-of-the-line Huawei Mate 20 Pro. The president of the company's smartphone division, He Gang, made the announcement on his verified Weibo page (via GizmoChina). This special edition will be dressed in emerald and feature 8GB of RAM and 256GB of storage (matching the most expensive version of the phone already available). Huawei will also offer a commemorative version of the Huawei Nova 4 in Secret Red.
Both models come with a special logo on the back that commemorates the 200 million Huawei phones shipped this year. Pricing has not been announced, but both models will be available in China starting on January 1st at 10:08 am local time. You can bet that the hundreds of Chinese companies offering subsidies to employees who buy Huawei phones will be happy to shoulder some of the costs of these two special editions.
Off topic- why's there no Christmas wishes to readers from Phonearena?
Merry Christmas!! Maybe, they don't celebrate Christmas since it's not Christ's real birthday?


text:
Q: Error on Joomla Website after upgrading from PHP 7.4 to 8.0 Update 2:
Regarding the error "Call to a member function children() on null", I found these functions.
public function hasChildren()
{
    return $this->hasChildNodes();
}

public function children($query = null)
{
    $children = array();

    if (!$this->hasChildren()) {
        return $children;
    }

    if ($query == null) {

        foreach ($this->childNodes as $child) {
            if ($child->nodeType == XML_ELEMENT_NODE) {
                $children[] = $child;
            }
        }

        return $children;
    }

    return $this->query(CssSelector::toXPath($query, 'child::'));
}

public function removeChildren()
{
    while ($child = $this->firstChild) {
        $this->removeChild($child);
    }

    return $this;
}

#########################################
Update:
I tried to change the code to
public function before(...$data): void
    {
      foreach($data as $item) {

        $item = $this->prepareInsert($item);
        $this->parentNode->insertBefore($item, $this);

     }
 }

This seems to work, but I get more of those errors. At one point I changed the code from:
public function prepend($data)
{
    $data = $this->prepareInsert($data);

    if (isset($data)) {
        if ($this->hasChildren()) {
            $this->insertBefore($data, $this->firstChild);
        } else {
            $this->appendChild($data);
        }
    }

    return $this;
}

to this:
public function prepend(...$data): void
{
    foreach($data as $item)
    {
        $item = $this->prepareInsert($item);

        if (isset($item)) {
            if ($this->hasChildren()) {
                $this->insertBefore($item, $this->firstChild);
            } else {
                $this->appendChild($item);
            }
        }
    }
}

Now, I get on my page the error message:
Call to a member function children() on null

There are no other information.

we have installed Joomla 3.10.10 and use the template "Effortless" from BDThemes (which we bought a long time ago via Envato). The template is based on the Warp 7 framework. However, our version is outdated and can no longer be updated, as the template is no longer available on Envato. Currently we are still using PHP 7.4, when we upgrade to PHP 8.0 we get the error message:
"Fatal error: Declaration of Warp\Dom\Element::before($data): void must be compatible with DOMElement::before(...$nodes): void in /homepages/13/d238860405/htdocs/homecms_ta/templates/effortless/warp/src/Warp/Dom/Element.php on line 108"
The code:
 public function before($data)
    {
        $data = $this->prepareInsert($data);
        $this->parentNode->insertBefore($data, $this);

        return $this;
    }

Unfortunately, I don't know how to fix it. I would be very grateful for any help.

A: There are some newer methods of Element (not available during the age of IE), for example:

*

*https://developer.mozilla.org/en-US/docs/Web/API/Element/after

*https://developer.mozilla.org/en-US/docs/Web/API/Element/before

*https://developer.mozilla.org/en-US/docs/Web/API/Element/prepend

*https://developer.mozilla.org/en-US/docs/Web/API/Element/append
Apparently newer versions of DOMElement PHP tried to follow it too.
All of those are variadic, but the old code of the theme may have assumed that you only had one element to insert.
The easiest way to go around it (minimal change) is probably to use a variadic argument ...$your_variable_name as $data, then use foreach($your_variable_name as $data){...} around your data. And we have to see if there are other side effects (if someone ever uses $element -> before($oneThing) -> before($anotherThing), the second one would fail (as the return type of the first before is void, unlike the old return of $this where you can use ->before directly after that).
The return $this probably won't get used (I'm not sure about that, though).
For example:
before
public function before(...$nodes): void
{
    foreach($nodes as $data){
        $data = $this->prepareInsert($data);
        $this->parentNode->insertBefore($data, $this);
    }
   // return $this;
}

prepend
public function prepend(...$nodes): void
{

    foreach($nodes as $data){
        $data = $this->prepareInsert($data);
        if (isset($data)) {
            if ($this->hasChildren()) {
            $this->insertBefore($data, $this->firstChild);
            } else {
                $this->appendChild($data);
            }
        }
   }
   // return $this;
}

(note that I can't test it myself as I don't have the complete code of the template you used)

redpajama_set_name: RedPajamaStackExchange


text:
ALL CATS ARE GREY
Installation of 6 sculptures during a performance at Heimathafen Neukölln "ARBEITEN KANNSTE SELBER" with Solistenensemble PHØNIX16 featuring performance duo Timo Kreuser and Guillaume Cailleau, with works by Kreuser/Cailleau, Vinko Globokar, Olga Neuwirth, and Luigi Nono.
The cats are modified Maneki-neko "lucky waving cats", which are often seen in Chinese or Japanese businesses to help bring in, for example, more customers and more money. These cats depict characters real and fictional that are usually considered either distinctly Evil or Good, but which could, depending on context, also be considered the opposite.
Materials: Plastic, polymer clay, acrylic paint. The cats waved their arms during the performance and some were fitted with mics to pick up the faint sound of the waving mechanism, which was audible during the performance. More photos of the installation to come.


I wholeheartedly recommend qsuk to any business considering outsourcing their HR function. Most recently, with their support, our organisation successfully defended a legal claim; qsuk's preparation for the Hearing was systematic and thorough and drew on the robust policies and documentation that they'd implemented previously. The team at qsuk is professional, reliable, efficient, and they respond quickly. They've taken the time to really get to know staff and understand our needs, they're evidently enthusiastic about their areas of expertise, and deliver the service positively and cheerfully.
qsuk ltd was recommended to SMART Systems to provide HR support. It's good to know that qsuk is ensuring we're fully compliant with employment legislation, which lets us concentrate on our business. With their support and practical advice, we've been able to make the staff changes we've wanted to. We've found the service friendly, reliable and professional.
Bramley Village Bakery has worked with qsuk ltd for the past five years. The team at qsuk advise us on Health & Safety, Food Safety, Quality Assurance, as well as HR matters. With their support, we've been able to develop our business with the confidence of knowing that everything is legally compliant. qsuk keeps us up to date on what we need to know, and any time we want advice, they are no more than a phone call away. Top notch service that we couldn't do without.
I felt that the training covered all bases and was very useful. I also felt that Flemming's delivery of the material was good as let's face it, Health and Safety is not the most exciting subject to talk about but he made it palatable and easy to understand.
In regards to the health and safety workshop – I think it was brilliant. Flemming is fantastic at giving the exact information required in a concise and easy to digest manner. I found myself engaged throughout and can remember pretty much everything we went through. There wasn't a single time I found myself bored or my mind drifting, which can on occasion happen if I am honest! The folder is superb and is already being filled in and used and will be a definite working tool in the store.


text:
Volvo Reveals 40 Series Entry Level Models After Days of Teaser Images
The new marketing trend is to make good use of social media websites and Volvo did a good job by releasing teaser images on Snapchat.
After days, the company has officially launched the concept for their 40 series entry level models.
The concept cars are named as 40.1 and 40.2 which we assume are tentative titles and will be renamed before official launch. They are set to be priced below the next gen 60 series and equipped with features that are fit for an entry level model. It is constructed on the popular CMA platform. The particular platform was conceived and designed by Volvo engineers in association with their parent company named Geely.
Volvo is set to launch the XC40 crossover and a brand new sedan. Both these concept cars are in their final stages after which the production version will be finalized. The CMA platform is specifically designed for smaller cars. It helps increase stability, center of gravity and promote best fuel efficiency. The versatile platform can not only readily accommodate petrol and gasoline engines but is also an apt fit for hybrid as well as electrified cars. The automobile manufacturer confirmed that they have some ambitious plans for the next few years. The idea is to create cars which can compete against luxury models from their immediate rivals.
"The brand has always been ahead of its competitors and we have set a new benchmark by creating a new vehicle architecture combined with an efficient powertrain. The innovation has helped us leap miles ahead of our competitors in the premium segment. With the development of the new battery electric powertrain, we are confident that a bright future awaits Volvo in the automobile segment," said Peter Mertens, the company's senior vice president in the research and development segment.
Volvo has confirmed that the brand will be ready with its fully electrified vehicle by 2019. Tesla, the pioneers in the field of EVs has already launched the Model 3 which goes on sale in 2018. When the world of automobiles shifts towards battery powered cars, Volvo will be ready to face the competition and deliver competent cars.
The CMA platform will play an integral role in helping them accomplish the feat. The base 40 series will be equipped with multiple safety features including city safety, pedestrian detection, adaptive cruise control, pilot assist, cyclist detection among other similar features for easy driving.
2018 VolvoVolvoVolvo 40 Series
The German automaker BMW is working on its 2024 BMW M3 CS as part of
Mazda is all set to make a complete revelation of its upcoming 2024 Mazda CX-90
Volvo, the luxury car manufacturer, has released some details of its 2024 Volvo XC40 Recharge
Bentley is working on the development of its 2025 Bentley Continental GT. The development of
The 2024 Tesla Model 3 was recently spotted on the road for testing with camouflage.
2024 Mercedes Benz EQG Spy Photos Reveal its Interiors
As the luxury car manufacturer Mercedes-Benz is making its transition from gas-powered cars to electric


"Decrease in Central Venous Catheter Placement and Complications Due to" by Arthur K Au, Masashi Rotte et al.
Poster presented at: American College of Emergency Physicians (ACEP) conference.
Au, Arthur K; Rotte, Masashi; Grzybowski, Robert; Ku, Bon; and Fields, Jason M., "Decrease in Central Venous Catheter Placement and Complications Due to Utilization of Ultrasound-Guided Peripheral Intravenous Catheters" (2012). Department of Emergency Medicine Faculty Papers. Paper 14.


Earlier this year I wrote about the recent rise in popularity of the sweet potato. I attributed the 80% increase in consumption of sweet potatoes in the U.S. between 2000 – 2014 (source) to the emergence of the Paleo Diet. Before the Paleo diet even made it into modern-day vernacular, sweet potatoes were a regular Thanksgiving Day staple, even though they were often referred to by another name.
Multiple varieties of sweet potatoes have been grown in the United States since colonial times. In order to differentiate the different types, farmers used the term "yam" which was derived from the name of a root vegetable native to Africa that closely resembled the sweet potato. This was the start of the culinary name game and eventually led to the USDA including "sweet potato" on the label of yams sold in the US (source).
If you really want to include yams in your Thanksgiving, you'll have to hit up the international supermarkets. It may be worth the trip because real yams do have some nutritional advantages over their starchy doppelgänger.
Ultimately, if you're looking for foods lower on the glycemic index, you'll want to seek out true yams. That may be a good idea on Thanksgiving considering Americans consume an average of 3000 calories during Thanksgiving dinner alone (source).
A few tricks you can utilize to avoid holiday binge eating include chewing your food more thoroughly, putting your fork down between bites, not going back for seconds and completing the following workout before sitting down for your Turkey day feast.
This workout focuses on your core, which is another reason you'll want to complete it BEFORE you eat dinner on Thanksgiving. I recommend performing the following exercises in superset format, which requires you to complete a desired number of repetitions for 3 separate exercises in succession.
Supersets allow you to up the intensity of your workout in a shorter period of time. A shorter, more intense workout will give you more time to spend with friends and family. Just make sure you warmup and modify the workout to match your fitness level.
Let us know in the comment section below if you completed this or any pre-holiday workout. ENJOY & HAPPY THANKSGIVING!
I didn't get my weekly "What's on the Menu" post done for its normal Thursday post date, but I still wanted to share it with you. Read about my experience with intermittent fasting then enjoy another effective weekend workout.
I was first introduced to the idea of fasting during my formative years in Catholic elementary school. Every Friday during Lent (the 40 days leading up to Easter), all Catholics were encouraged to fast during the day and then finish the day with a "meatless" dinner. Thankfully the Bible didn't consider seafood meat, which meant I enjoyed a lot of McDonald's fish sandwiches and pizza for dinner during Lent.
I'll admit that my dedication to daylight fasting during Lent was spotty at best and, as devoted to Catholicism as my parents were and still are, they didn't send my brother and I to school without lunches. I was extremely grateful to them at the time, but with what I know now, periodic fasting could have been extremely beneficial.
The origins of fasting date back to ancient Greece and it's inclusion in numerous religious doctrine make it one of the oldest weight loss/control methods. Even though its been used for several millennia, the extent of fasting's metabolic benefits are just starting to be discovered (source).
One of my go-to sources for the latest health research, Dr. Rhoda Patrick, has been promoting the benefits of intermittent fasting, which she refers to as time restricted eating, for some time now. The basic concept is that you have an eating window everyday that syncs up to your natural circadian rhythm. The research suggests that the most metabolic benefits occur with a eating window of no more than 12 hours and, unlike my Lenten fasts, occurs during the day (source).
I've been partaking in time restricted eating for the past 3 weeks and I'll admit it's pretty tough for someone like me. I have a very active job and some days I leave the house before 7am and don't return till 8pm. Thankfully I've been very good at packing a lunch full of nutritious and satiating foods that help me get enough fuel in during my eating window.
Even though I started my current intermittent fasting plan with no desire to lose weight, I've lost nearly 5 lbs in 3 weeks. I know that doesn't sound like a lot but when you're 5'11" and 160, losing 5 lbs without really trying is pretty significant. As great as the weight loss is, I'm more excited by the possibility that this way of eating can help me prolong my life.
Another way to prolong your life is with regular exercise, which is why you should try the weekend workout featured below. This workout includes several variations of one of the most beneficial exercise there is, the squat.
Squats are considered a compound exercise, which means they are multi-joint movements that require the use of various muscle groups. Try to knockout these various forms of the squat and make sure you let us know in the comment section below or on social media (Facebook, Instagram or Twitter) how you feel the next day. Don't forget to warmup and modify the workout to match your fitness level. ENJOY!
The worse thing about dietary fat is that it's called FAT!
That one statement inspired me to look into the low-carb, high-fat (LCHF) lifestyle to determine if it suited me better than the not so low carb lifestyle I was participating in at the time. After subtracting certain items that contain refined carbs from my diet and adding more items that were high in healthy fats, I started feeling fuller, longer and was no longer hangry two hours after a meal.
There is one particular "fatty" food item that has been a part of my diet well before my shift to LCHF. I've been hearing about its health benefits for well over a decade and its versatility has made it a staple in Shannon and I's kitchen. It can be used as a cooking oil, salad dressing, finishing sauce and even a skin care product. The multi-talented food item I'm referring to is olive oil and it's this week's menu spotlight.
Olive oil is a broad category of oil made from pressed olives. I realize that isn't "breaking news," but I wanted to mention that because the different types of olive oils at the supermarket can be quite overwhelming. If you're looking for the variety that provides the most health benefits, you'll want to stick with extra virgin olive oil (EVOO). Any other variety may use solvents to extract the oil or partially consist of cheaper, inflammatory oils.
Even though EVOO, purchased from a reputable producer, doesn't contain any protein or carbs, it's still highly nutritious. One hundred grams, which is about 7 tablespoons, of EVOO contains 72% of our recommended daily allowance (RDA) for Vitamin E and 75% of our RDA for Vitamin K (source), both of which can contribute to preventing cardiovascular disease. The micronutrients contained in olive oil are impressive but it's the type of fat it contains that really sets it apart from other cooking oils.
EVOO consists primarily of monounsaturated fat. This type of fat is more heat-resistant, which means it is less likely to oxidize when used in cooking applications. This is one aspect of EVOO that makes it superior to other cooking oils like canola or even flax-seed, which consist primarily of polyunsaturated fat. Less oxidation means less free radical production, which can cause inflammation that may researchers believe is responsible for chronic health conditions like atherosclerosis, Alzheimer's and cancer. Oh, and EVOO contains a ton of anti-inflammatory phenols and polyphenols to further combat those previously mention conditions (source).
As you can imagine, I frequently use EVOO to saute veggies and as my go-to salad dressing (2 parts EVOO + 1 part vinegar). I also use it to make my baked sweet potatoes fries nice & crispy, add extra flavor to my fried eggs and add even more monounsaturated fat to my daily avocado snack.
I mentioned it quickly earlier in this post, but it is very important that you purchase your EVOO from a reputable producer to get the optimum amount of health benefits. There are two great books, Extra Virginity & Real Food / Fake Food, that describe some of the deception associated with olive oil.
A couple quite tips I'll give you in regards to purchasing EVOO are buy imported and make sure the container it comes in is NOT clear (light can cause oxidation over time). If you have a brand of EVOO that you swear by, I'd love to hear about it. Feel free to share it with us via email (elementaltampa@gmail.com) or snap a pic of the bottle and share it on our social channels (Facebook, Instagram or Twitter) and don't forget FAT DOESN'T MAKE YOU FAT!


text:
\section{Introduction}

Identifying intermediate-mass black holes (IMBHs; $M_{\rm{BH}}=10^2-10^5$~M$_{\odot}$) or their hosts is not straightforward \citep{Miller:2004uq}. The observational examples that are closest to this IMBH mass range are often termed as massive black holes (MBHs) and often considered to be in a range of $10^5-10^7$~M$_{\odot}$ \footnote{The term IMBH is used in the ULX community while the term MBH is used in the AGN community and these mass ranges are blurred together in the $10^4-10^6$~M$_{\odot}$ range. However, the low end of the IMBH range is physically motivated as BHs above 100~M$_{\odot}$ are hard to form from a single star. Also, one may want to avoid the usually considered lower range of supermassive BHs of $10^6$~M$_{\odot}$.}. Among these MBHs, NGC 4395 has the lowest mass black hole (BH) of $M_{\rm{BH}}=(3.6\pm1.1)\times10^5$~M$_{\odot}$ \citep{Peterson:2005uq}, that is obtained from reverberation mapping. There are several other examples of MBHs with mass estimates either based on their accretion properties \citep[e.g.][]{Reines:2011uq,Kamizasa:2012oq,Secrest:2012kx,Nyland:2012zr,Reines:2014ly} or are virial mass estimates \citep[e.g.][and references therein]{Greene:2004fk,Barth:2004qf,Seth:2010nx,Schramm:2013vn,Reines:2013ys}. The majority of these MBHs are found (or looked for) in dwarf and bulgeless galaxies. Due to the peculiar hosts and the relatively low BH masses, the non-accretion based methods may start to fail below $\sim10^5$~M$_{\odot}$ \citep[e.g.][]{Reines:2013ys}. On the other hand, a few of the MBHs were studied in the radio band \citep[e.g.][]{Wrobel:2006tg,Wrobel:2008hc,Reines:2011uq,Nyland:2012zr,Secrest:2013fv,Reines:2014ly,Paragi:2014uq} and in all cases the radio emission is likely due to BH activity.

Observable IMBHs have been proposed \citep[e.g.][]{Kaaret:2001ya,Miller:2004kx} in the context of ultraluminous X-ray sources (ULXs; $L_X>3\times10^{39}$~erg~s$^{-1}$) as well as in globular clusters (GCs) \citep[e.g.][and references therein]{Miller:2002rq,Maccarone:2004cq}. ULXs are non-nuclear X-ray sources with a luminosity exceeding the Eddington-limit of a $20-M_{\odot}$ BH, residing in external galaxies. However, most of the ULX population might be explained by mechanical beaming \citep[e.g.][]{King:2009ys}, super-Eddington accretion \citep[e.g.][]{Begelman:2002fb,Poutanen:2007vn}, and massive stellar-mass BHs \citep[e.g.][]{Zampieri:2009if,Belczynski:2010kx}. Relativistically beamed X-rays has also been proposed \citep{Kording:2002xz}, that is difficult to reconcile with the X-ray spectral behaviour of ULXs (see later). Whether there is a link between bulgeless galaxies, dwarf galaxies, and ULXs is still an open question \citep[e.g.][]{Somers:2013ve,Prestwich:2013bh,Plotkin:2014fk}.

A sub-class of ULXs, called Hyperluminous X-ray sources (HLXs), have X-ray luminosities of $L_X \geq 10^{41}$~erg~s$^{-1}$. Their luminosities deem them to be the best candidate IMBHs among ULXs as the above mechanisms can not coherently explain such a powerful output from a stellar-mass BH. However, so far only a handful of HLXs have been studied \citep[e.g.][]{Kaaret:2001ya,Gao:2003fk,Farrell:2009ys,Sutton:2012kx}. The record-holder is HLX-1 in ESO 243-49 with its peak X-ray luminosity of $L_X\simeq10^{42}$~erg/s with a BH mass of $M_{\rm{BH}}\simeq(0.3-30) \times 10^4$~M$_{\odot}$ \citep{Davis:2011oq,Godet:2012ys,Webb:2012kx,Straub:2014fk}. HLX-1 was proposed to be the core of a tidally stripped dwarf \citep{Farrell:2012vn,Farrell:2014cr} or a bulgeless satellite galaxy \citep{Mapelli:2013dq}. \citet{Lasota:2011fk} proposed that HLX-1 may be a binary system with an eccentric orbit. In this case, the BH accretes material from a donor star when it passes periastron, which is thought to drive HLX-1 into regular X-ray outbursts. A wind fed binary system might also be a viable explanation \citep{Miller:2014bs}.

 The X-ray behaviour of HLX-1 is remarkably similar to BH X-ray binaries (BHXRBs) \citep[e.g.][]{McClintock:2006fv,Fender:2009bh}. It shows X-ray state transitions \citep{Godet:2009yj} and follows the standard disk law between disk luminosity and temperature ($L\propto T^4$) in its soft state \citep{Servillat:2011fd,Godet:2012ys}. In contrast, the majority of the ULXs may be in a distinct  or ``ultraluminous" X-ray state \citep[e.g.][]{Feng:2009wq,King:2009ys,Gladstone:2009fk}, however, see also \citet{Miller:2013fk} for a number of ULXs that are broadly consistent with the standard disk law. That said, there is one other HLX, M82 X-1, that also follows the trend of $L\propto T^4$ \citep{Feng:2010fk}.

Radio sources offer the best testbed for the scale invariance of the jets under BH mass and/or accretion rate \citep{Heinz:2003fk} and for the disk-jet coupling \citep[e.g.][]{Falcke:1995yb,Merloni:2003ri,Falcke:2004wm}. Although, radio emission as a signature of an accreting IMBH in GCs is yet to be discovered \citep[e.g.][and references therein]{Cseh:2010vn,Wrobel:2011qf}. {On the other hand,} \citet{Webb:2012kx} found that HLX-1 exhibits radio flares (or jet ejections) when the source transits from a hard to soft X-ray state, similar to the behaviour of BHXRBs. \citet{King:2013ij} also found similarities to BHXRBs in NGC 4395 in a sense that its disk-jet coupling could belong to the so-called outliers \citep[e.g.][]{Coriat:2011qm} on the radio-X-ray luminosity plane.

In this paper we present radio observations of HLX-1 during its X-ray hard state with the Australia Telescope Compact Array (ATCA) as well as follow-up observations of its flaring emission during its outburst with the Karl G. Jansky Very Large Array (VLA). Throughout this paper, we use a spectroscopically measured distance of HLX-1 of 95~Mpc \citep{Wiersema:2010zr}.

\begin{table*}
\caption{Summary of observations \label{obs}}
\begin{tabular}{ccllclcc}
\hline\hline
Array&Array&Observation&On-source&Central&Reached&Flux&HLX-1 outburst\\
&configuration&date&time&frequency&rms noise& density&status\\
\hline
VLA&A&2011 Aug 23&1 hr&5.9 GHz&7 $\mu$Jy/b&$\leq$21 $\mu$Jy&during burst\\
\hline
ATCA&6D&2012 May  26&7.5 hr&6.7 GHz&7 $\mu$Jy/b&24$\pm$7 $\mu$Jy&hard state\\
ATCA&6D&2012 May  27&7 hr&6.9 GHz&8 $\mu$Jy/b&29$\pm$8 $\mu$Jy&hard state\\
ATCA&6D&2012 May  28&7 hr&6.9 GHz&7 $\mu$Jy/b&$\leq$21 $\mu$Jy&hard state\\
ATCA&6A&2012 Aug 19&9 hr&6.7 GHz&7 $\mu$Jy/b&25$\pm$7 $\mu$Jy&hard state\\
Combined&--&May-Aug&30.5 hr&6.8 GHz& 3.3 $\mu$Jy/b&22$\pm$5 $\mu$Jy&hard state\\
Combined&--&May-Aug&30.5 hr&5.5 GHz& 3.7 $\mu$Jy/b&23$\pm$5 $\mu$Jy&hard state\\
Combined&--&May-Aug&30.5 hr&9.0 GHz& 5.8 $\mu$Jy/b&19$\pm$8 $\mu$Jy&hard state\\
\hline
VLA&B&2012 Sep 1&1 hr&9 GHz&6 $\mu$Jy/b&$\leq$18 $\mu$Jy&during burst\\
VLA&B&2012 Sep 3&1 hr&9 GHz&6 $\mu$Jy/b&$\leq$18 $\mu$Jy&during burst\\
VLA&B--$>$BnA&2012 Sep 5&1 hr&9 GHz&6 $\mu$Jy/b&$\leq$18 $\mu$Jy&during burst\\
VLA&BnA&2012 Sep 23&1 hr&5.5 GHz&6 $\mu$Jy/b&$\leq$18 $\mu$Jy&burst decay\\
VLA&BnA&2012 Sep 24&1 hr&5.5 GHz &7 $\mu$Jy/b&$\leq$21 $\mu$Jy&burst decay\\
VLA&BnA--$>$A&2012 Sep 25&1 hr&5.5 GHz&7 $\mu$Jy/b&$\leq$21 $\mu$Jy&burst decay\\
VLA&A&2012 Oct 1&40 min&5.5 GHz&9 $\mu$Jy/b&$\leq$27 $\mu$Jy&burst decay\\
Combined VLA&--&2011-2012&7.66 h&7.25 GHz&2.1 $\mu$Jy/b&$\leq$6.3 $\mu$Jy&during burst\\
Combined VLA, 60 k$\lambda$&--&2011-2012&7.66 h&7.25 GHz&3.1 $\mu$Jy/b&$\leq$9.3 $\mu$Jy&during burst
\end{tabular}
\medskip

The table shows the individual and combined observations of HLX-1 carried out with the VLA and the ATCA, the array configuration, and the date of the observations. We list the reached rms noise levels at the corresponding central frequency. The table also shows the flux densities obtained from modelling the visibilities or the 3-$\sigma$ upper limits that correspond to a point source. The last column reflects the status of the outburst of HLX-1. The point source flux densities were estimated from the peak brightnesses for the cases of individual detections.
\end{table*}

\section{Observation, Analysis, and Results}

\begin{figure*}
\rotatebox{0}{\resizebox{7.2in}{!}{
\includegraphics{Fig1.ps} } }
\caption{The figure shows the evolution of the  2010, 2011, and 2012 outburst of HLX-1 along with radio measurements. {\bf The top} panel shows the {\it Swift} X-ray light curve with count rates in the $0.3-10$~keV band. The ticks above each outburst indicate the epochs of radio observations. {\bf The middle} panel shows the corresponding radio measurements. Detections are indicated with dots and non-detections are shown with an arrow. The non-detection values correspond to 3-$\sigma$ upper limits using the rms noise level. {\bf The bottom} panel also shows the same radio data, but with zoomed subsets for clarity. The first subset correspond to the 2010 outburst, the second subset to the 2011 outburst. The third subset shows observations from May 2012, while the fourth subset shows the data corresponding to the 2012 outburst. The bottom panel also shows the deepest 3-$\sigma$ VLA upper limit. Radio points are drawn from Table \ref{obs} and from \citet{Webb:2012kx}.}
\label{lc}
\end{figure*}

\subsection{{\it Swift} X-ray light curve}

The X-ray light curve of HLX-1 is shown in Fig. \ref{lc}, indicating the evolution of the  2010, 2011, and 2012 outburst in the 0.3-10 keV band together with radio measurements of HLX-1 of this paper and from \citet{Webb:2012kx}. The X-ray light curve was adapted from \citet{Webb:2014fk} and for data reduction and analysis we refer to \citet{Godet:2012ys,Webb:2014uq}. HLX-1 has a fast rise exponential decay (FRED) type of X-ray light curve and the source rapidly transits from a hard to soft state within days, right after the onset of the outburst. After reaching the peak X-ray luminosity, it begins a decay to quiescence over a timescale of months with decreasing duration \citep[e.g.][]{Godet:2014fk}.

\subsection{ATCA observations}\label{atcaob}

We obtained radio observations to look for further similarities between HLX-1 and the phenomenology of BHXRBs, that are known to show flat-spectrum radio cores during their X-ray hard state and are known to show radio flares which are associated with their X-ray state transitions \citep[e.g.][]{Fender:2009bh}. The ATCA measurements were obtained during the hard state of HLX-1 \citep{Godet:2012ys,Webb:2014uq}. So, we combined all of our ATCA data from May and Aug 2012 (see Sec. \ref{atcaob}). The rest of the radio measurements, shown in Fig. \ref{lc}, were obtained during one of the X-ray outbursts of HLX-1 when the source was in a soft state \citep{Servillat:2011fd,Godet:2012ys}, following an X-ray state transition. We obtained the VLA data during the 2011 and 2012 outburst to catch potential flaring events, and then we combined these observations according to the X-ray state of HLX-1 (see Sec. \ref{vlaob}).

\begin{figure*}
\rotatebox{270}{\resizebox{3.2in}{!}{
\includegraphics{Fig2.ps}}}
\rotatebox{270}{\resizebox{3.2in}{!}{
\includegraphics{Fig3.ps}}}
\caption{{\bf Left:} The combined ATCA image of HLX-1 during the X-ray hard state at 6.8~GHz central frequency. The circle with a cross shows the 95\% positional uncertainty of the Chandra \& HST counterpart of HLX-1 with a radius of 0.5" \citep{Farrell:2012vn}. The radio image was made using natural weighting. The contours are drawn at $9.9 \times (\sqrt{2})^{n} \mu$Jy beam$^{-1}$. The lowest contours represent radio emission at $\pm3$ times the rms noise level of 3.3~$\mu$Jy beam$^{-1}$. The peak brightness is 119~$\mu$Jy~beam$^{-1}$. The Gaussian restoring beam size is $2.79" \times 1.53"$ at a major axis position angle of 10$^\circ$. {\bf Right:} The combined VLA image of the region of HLX-1 showing its host galaxy, ESO~243-49, at 7.25~GHz central frequency. The circle with a cross shows the 95\% positional uncertainty of the Chandra \& HST counterpart of HLX-1 with a radius of 0.5". The radio image was made using natural weighting. The contours are drawn at $6.3 \times (\sqrt{2})^{n} \mu$Jy beam$^{-1}$. The lowest contours represent radio emission at $\pm3$ times the rms noise level of 2.1~$\mu$Jy beam$^{-1}$. The peak brightness is 69~$\mu$Jy~beam$^{-1}$. The Gaussian restoring beam size is $2.40" \times 0.76"$ at a major axis position angle of --3$^\circ$.}
\label{HS}
\end{figure*}

We observed HLX-1 at a location of 1$^h$10$^m$28$^s$.28, $-46^{\circ}$~4'~22".3 \citep{Webb:2010dq,Farrell:2012vn} with the CABB-upgraded \citep{Wilson:2011lg} ATCA in configuration 6D and 6A (baselines up to 6 km) in 2012 under program code C2361 (PI Webb). The data were taken using the CFB 1M-0.5k correlator setup with 2 GHz bandwidth and 2048 channels, each with 1 MHz resolution; and with central frequencies of 5.5 GHz and 9 GHz simultaneously. The on-source integration times were 7-9~hr, see Table~\ref{obs} for more details. The primary amplitude calibrator was PKS~1934-638 and the phase calibrator was 0048-427. The primary was observed for 10 min and the secondary was observed every 15 min. The data reduction was performed using the Miriad software package \citep{Sault:1995lo}.

First, we combined the 5.5 GHz and 9 GHz visibility data to enhance sensitivity at each epoch. Then, we further combined the observations from May and Aug 2012 as these observations were carried out in the low/hard state of HLX-1 to reach the best sensitivity. Furthermore, we made a separate combination of these data in each frequency band. To produce images we used the multi-frequency synthesis (MFS) method \citep{Sault:1999zr} and the measured system temperatures to compute the weight of the visibility points by the inverse noise variance (instead of integration time). The images were made without self-calibration and with natural weighting.

The resulting rms noise levels are listed in Table~\ref{obs}. We detected HLX-1 on 26, 27 May and on 19 Aug with a peak brightness of $24\pm7$, $29\pm8$, and $25\pm7$~$\mu$Jy~beam$^{-1}$, respectively. (The 3-$\sigma$ upper limit of 21~$\mu$Jy~beam$^{-1}$ on 28 May is consistent with the above values within the errors). Due to the low signal to noise ratios, the point source flux densities, listed in Table~\ref{obs}, were estimated from the peak brightnesses for the cases of individual detections. The resulting image from the combined data of May and Aug 2012 is shown in Fig. \ref{HS}. In this deepest ATCA image, we detected emission at the location of HLX-1 during the hard state with a signal to noise ratio of $\sim$5.5 with a peak brightness of $18\pm3.3$~$\mu$Jy~beam$^{-1}$. We fitted both, a point-source model and a Gaussian that resulted in $S_{\nu,\rm{Point}}=22\pm3.5$~$\mu$Jy and $S_{\nu,\rm{Gauss}}=26.5\pm5.5$~$\mu$Jy that are consistent within the errors. A point-source model adequately describes the radio emission. However, without higher resolution observations it is not possible to distinguish between a point source or an extended source. We note that the combination of the ATCA data and the VLA data or the combination of the hard-state data with non-hard state data are beyond the scope of this paper.

To test the fitted values and to minimise the error we attempted to fit the data on the visibility plane. To this purpose we used the Miriad task {\sc uvfit}. First, we attempted to fit the individual epochs, however, due to the low signal to noise ratio the fit did not converge. Regarding the combined data in the individual bands, we fit a point source to HLX-1 and a Gaussian to the host galaxy simultaneously and found $S_{\nu}$=23$\pm$5 $\mu$Jy at 5.5~GHz and $S_{\nu}$=19$\pm$8 $\mu$Jy at 9~GHz. For the deepest ATCA data at 6.8 GHz, we found $S_{\nu}$=22$\pm$5 $\mu$Jy for HLX-1.

\subsection{VLA observations}\label{vlaob}

We observed HLX-1 using the VLA in 2011 and 2012 under project code 11A-290 (PI Krauss) and 12B-024 (PI Cseh), with filler scheduling priority. The observations were carried out in B, A, or hybrid array configuration in X or C band, see Table \ref{obs} for more details. The typical total on-source time was 1~hour that is limited by the low declination of the target. The total bandwidth was 2~GHz, covering either 8--10~GHz (X band) or 4.5--6.5~GHz (C band), that consists of two base bands with 8-bit sampling, each with 8 sub-bands with 4 polarisation products, 64 channels per sub-band with 2~MHz channel width. In 2011, the lower and the upper baseband was placed as 4.5--5.5 and 6.2 --7.2~GHz.

The data were calibrated and imaged in CASA 4.1.0  \citep{McMullin:2007ys} and we applied the VLA calibration pipeline version 1.2.0. \footnote{https://science.nrao.edu/facilities/vla/data-processing/pipeline} We used 3C48 for absolute flux density and bandpass calibration, and J0106-4034 was used for antenna gain and phase calibration. The primary calibrator was observed for 10 min and the phase calibrator for 2 min out of every 10 min. Images were made at each epoch using the MFS method and natural weighting. There was no self-calibration applied. The pipeline calibration products and the image quality -- i.e. the reached rms noise levels and noise structures -- were then visually examined. We also compared these to a set of manually calibrated data, and found equally good or better image quality of the pipeline calibrated data due to a more robust flagging strategy.

Our primary aim was to detect radio flares, study their time evolution, and to test if there is a permanent emission, like a ULX radio bubble \cite[e.g.][]{Cseh:2012fk}, at low flux density levels. The individual runs are in principle suitable to look for flares from HLX-1. However, we did not detect emission at or above the 3-$\sigma$ rms level (that corresponds to the individual epochs, see Table~\ref{obs}) at the location of HLX-1 in these observations.

Furthermore, to test the presence of a permanent or an extended emission, all of the VLA visibility data were combined and then imaged to reach the best rms noise level so far. This is shown in Fig. \ref{HS} right, where no radio emission is detected at the location of HLX-1 above a 3-$\sigma$ upper limit of $\sim6.3~\mu$Jy. To test whether we could have resolved out large-scale, extended structures around HLX-1, we again combined all the visibility data and we restricted the maximum $(u,v)$ range to 60~k$\lambda$. This reduction of the apparent maximum baseline length produces a much larger synthesised beam width allowing for the detection of emission from a larger spatial scale. In practice, the largest angular scale (LAS) that can be imaged comes from the shortest baselines and for these array configurations and observing bands the LAS is 4.5-8.5 arcsec\footnote{https://science.nrao.edu/facilities/vla/docs/manuals/oss/\\performance/resolution}.  For our combined data, we take a conservative LAS of $\sim4.5$ arcsec that corresponds to A configuration in C band. The resulting synthesised beam width is 4.70"$\times$2.40", within the LAS, and the resulting rms noise level is 3.1 $\mu$Jy/beam. We do not detect radio emission at the location of HLX-1. The VLA data supports that there is no permanent or extended emission present smaller than a physical scale of 2.2 kpc $\times$ 1.1 kpc.

Here we also provide the peak brightness and the total flux density of the host galaxy of HLX-1 that is fitted with a Gaussian and the errors given are statistical. These values correspond to Fig. \ref{HS} left, right, and to the $(u,v)$-restricted VLA image. Furthermore, given the low elevation of our target, we attempt to quantify the potential atmospheric attenuation in X band. To this end, we compare the flux density and the fitted position of the host galaxy between the ATCA and the VLA at 9~GHz central frequency. We combined all of the VLA data observed in X band and restricted the $(u,v)$ range to 60~k$\lambda$ to minimise the flux density loss due to the higher resolution of the VLA. Comparing the flux densities, we find that they agree within the statistical errors (Table \ref{host}). However, given the relatively high uncertainties on the fitted flux densities and the lack of a more suitable source on the target field, we quote a conservative atmospheric attenuation of $<24$\% by taking the flux densities at face value and assuming a non-variable source. We also provide flux densities for the ATCA data, obtained from fitting a Gaussian on the visibility plane, that may indicate a flux density overestimate for the image-plane Gaussian fits and thus less of a difference at high frequencies. The fitted positions differ by only 0.02 arcsec in RA and 0.14 arcsec in Dec that is less than our cell size.

\begin{table}
\caption{Host galaxy radio properties}\label{host}
\begin{tabular}{cccccc}
\hline\hline
Array&Peak&Flux density&Beam&Freq.\\
&[$\mu$Jy/b]&[$\mu$Jy]&[" $\times$ "]&[GHz]\\
\hline
ATCA&119$\pm$9&157$\pm$16 (153$\pm$6)&2.79 $\times$1.53&6.8\\
VLA&68$\pm$4&116$\pm$9&2.40 $\times$0.76&7.25\\
VLA, 60k$\lambda$&100$\pm$7&122$\pm$12&4.70 $\times$2.40&7.25\\
ATCA&117$\pm$12&167$\pm$24 (143$\pm$11)&2.30 $\times$1.23&9.0\\
VLA, 60k$\lambda$&91$\pm$9&127$\pm$19&5.99 $\times$2.52&9.0\\
\end{tabular}
\medskip

The table shows the image-plane Gaussian fit results of the host galaxy. Flux density values in brackets indicate a Gaussian model fit on the visibility plane.
\end{table}

\subsection{Spectral index and variability}

We attempted to estimate a spectral index of the radio source detected with ATCA from the combined images in the different bands and found a two-point spectral index between 5.5 and 9 GHz of $\alpha=-0.4\pm1.0$, where $S_{\nu}\sim\nu^{\alpha}$. This spectral index does not constrain the radio spectrum to be steep, flat, or inverted.

We aimed to repeat this exercise on the previous individual detections in 2010 and 2011, using peak brightnesses in the different bands; see the values in the supplementary material of \citet{Webb:2012kx}. However, the frequency-split data do not show detections on 4 Sep 2011 due to the high noise level. Furthermore, in the remaining epochs, detections are present in only one of the frequency bands. Therefore one can set upper or lower limits to the spectral indices using 3-$\sigma$ upper limits from the counter band. We find spectral indices of $\alpha_1<-0.5\pm0.5$ on 2010 Sep 3, $\alpha_2<0.3\pm0.5$ on 2011 Aug 31, and $\alpha_3>1.6\pm0.4$ on 2011 Sep 3. The spectral index of $\alpha_1$ indicates a flat to steep spectrum, $\alpha_2$ does not constrain the radio spectrum, and $\alpha_3$ indicates an inverted radio spectrum. \citet{Webb:2012kx} showed that the radio emission in 2010 and 2011 was variable. Considering our deepest VLA limit and comparing it to the previously measured peak brightnesses, we find that the emission is variable by a factor of about ten, which unambiguously confirms a variable radio source in 2010 and 2011. The apparent variation in the spectral indices ($\alpha_1,\alpha_2,\alpha_3$) is also expected for a variable jet source.

Regarding the ATCA data in 2012, the peak brightness values are constant within the errors. Albeit, the non-detection on 28 May might indicate variability that is difficult to assess due to the high rms noise levels. However, in the deepest VLA limit the probed spatial scales are coupled with a sensitivity that is better than and matched to that of the ATCA, which argues against a permanent radio source in 2012.

\section{Discussion}

In the following, we discuss the radio emission detected at the location of HLX-1 during the hard state. First, we investigate whether this emission could be contaminated by permanent emission such as a radio bubble or star formation. Then, we discuss potential origins of the emission due to a compact jet or an interacting jet with the ISM. Furthermore, we discuss the properties of the flaring emission and compare with microquasars and active galactic nuclei (AGNs).

\subsection{Permanent emission: radio bubble or star formation?}\label{bubble}

The smallest resolvable angular scale is 0.76 arcsec (Fig. \ref{HS} right), that corresponds to a physical scale of $\sim$350~pc at 95~Mpc. Some of the largest microquasar and ULX radio bubbles, like S26 and IC 342 X-1 \citep{Soria:2010lt,Cseh:2012fk}, have a size of $\sim200-300$~pc and a high radio luminosity of $L_R\simeq2 \times 10^{35}$~erg/s that would correspond to $\sim$3~$\mu$Jy at a distance of HLX-1. These sources would not be resolved and would not reach our detection threshold. On the other hand, there is at least one peculiar example of an extended radio source, assumed to be associated with the ULX NGC 2276 3c, with a size of 650~pc and with an integrated flux density of 1.4~mJy at 33.3~Mpc \citep{Mezcua:2013uq} that would be detectable as well as resolvable if placed at 95~Mpc. This source was also inferred to be powered by an IMBH, that may allow a better comparison with HLX-1. Given the that one would have detected ample extended emission if similar to NGC~2276~3c, HLX-1 is unlikely to be associated with any radio bubble above a flux density level of 6.3~$\mu$Jy.

\citet{Farrell:2012vn} argued for the presence of a young star cluster hosting HLX-1. In the following we estimate the expected radio flux density due to star formation. We take a near UV (NUV) flux of 23.96$\pm$0.04 mag at wavelength of 2829.8 \AA \, that is obtained from {\it HST} photometry \citep{Farrell:2012vn}, which corresponds to a NUV luminosity of $L_{\rm{NUV}}=(1.08\pm0.04) \times 10^{40}$~erg/s. Assuming that all of this emission is stellar in origin, we estimate the star formation rate (SFR) using the relation of  $\log \dot{M_{\star}}/(\rm{M_{\odot}\, yr^{-1}}) = \log L_{\rm{NUV}}/(\rm{erg\, s^{-1}}) - 43.17$ \citep{Kennicutt:2012kx}. Given that the accretion disk is expected to significantly contribute to the NUV emission, we place an upper limit to the SFR and find that $\dot{M_{\star}}\leq7.3 \times 10^{-4}$~M$_{\odot}$~yr$^{-1}$.

Using our SFR estimate, the expected thermal and non-thermal radio flux density can be obtained \citep{Murphy:2011vn,Nyland:2012zr} from
\begin{equation}
\begin{split}
& \left(\frac{L_{\nu}}{\rm{erg\,s^{-1} Hz^{-1}}}\right)=10^{27}\left(\frac{\dot{M_{\star}}}{\rm{M_{\odot}\, yr^{-1}}}\right) \times \\
& \left[2.18\left(\frac{T_e}{\rm{10^4\,K}}\right)^{0.45} \left(\frac{\nu}{\rm{GHz}}\right)^{-0.1}+15.1\left(\frac{\nu}{\rm{GHz}}\right)^{\alpha_{\rm{NT}}}\right],
\end{split}
\end{equation}
where we take $T_e=10^4$~K, $\alpha_{\rm{NT}}=-0.8$ and $\nu=7$~GHz. We find that the total radio flux density at 7~GHz due to SF would be $L_{\nu}\leq3.64 \times 10^{24}$~erg~s$^{-1}$~Hz$^{-1}$ that corresponds to a flux density of $\leq$0.34~$\mu$Jy at a distance of HLX-1. So, the ATCA radio emission is unlikely to be due to star formation or a radio bubble.

\subsection{Mass, accretion rate, and jet power}\label{jet}

We detected radio emission during the hard state with a total flux density of $S_{\nu}=22\pm3.5$~$\mu$Jy at a central frequency of 6.8~GHz at a significance of 5.5~$\sigma$. A point source model adequately describes the radio emission and it is unlikely to be permanent. Given that ``compact jets" are ubiquitous in a hard or inefficient accretion state and have a self-absorbed (flat or slightly inverted) radio spectrum, the radio emission detected at the location of HLX-1 can be consistent with a compact jet. Alternatively, this radio emission may not be related to the X-ray state of HLX-1 and it could perhaps be a residual emission due to the flaring activity of the source in a form that the ejected components could interact with the large-scale ISM. We discuss this option in the following sections. Here, we assume that the radio emission is causally connected to the X-ray hard state of HLX-1 and it is a compact jet as seen in other BHXRBs in this state.

Under this assumption, in the following we employ the ``fundamental plane" of BH activity \citep{Merloni:2003ri,Falcke:2004wm,Kording:2006pt,Plotkin:2012kx} to estimate the BH mass and use the flux density of the compact jet to estimate the accretion rate in the hard state, and total jet power. The correlation was found to be valid for hard X-ray state objects, where the accretion is jet-- or advection dominated, and with a small intrinsic scatter of 0.07 dex \citep{Plotkin:2012kx}. To estimate the BH mass we use the fit of \citet{Miller-Jones:2012uq}, who re-regressed the plane with the mass as the independent variable:
\begin{equation}
\log M_{\rm{BH}} = 1.638\log L_R - 1.136\log L_X -6.863.
\end{equation}
Here, $L_X$ is the X-ray luminosity in the 0.5-10 keV band and $L_R$ is the radio luminosity at 5~GHz (L=$\nu$L$_\nu$) in units of erg~s$^{-1}$ and the mass is in ${\rm M_{\odot}}$. The 1$\sigma$ uncertainty on the mass estimate is 0.44 dex. After substituting a typical hard state luminosity of HLX-1 of $L_X=(2.0\pm0.6)\times10^{40}$~erg~s$^{-1}$ \citep{Godet:2012ys} and $L_R=(1.2\pm0.3)\times10^{36}$~erg~s$^{-1}$, the BH mass would be $M_{\rm{BH}}=2.8^{+7.5}_{-2.1} \times 10^{6}$~M$_{\odot}$ at 90\% confidence. This is at least an order of magnitude higher than previous estimates (see later).

Similarly, under the assumption that we witness a compact jet, we derive a total jet power and an accretion rate using Eq. 1 and Eq. 2 of \citet{Kording:2008nq}. We obtain $Q_j\simeq7.2\times10^{36}[L_R/(10^{30}~\rm{erg/s})]^{12/17}\simeq1.4\times10^{41}$~erg/s and $\dot{M}\simeq4\times10^{17}[L_R/(10^{30}~\rm{erg/s})]^{12/17}\simeq7.8\times10^{21}$~g/s (or $1.2 \times10^{-4}$~M$_{\odot}$/yr).

Considering the jet power, we recall that the integrated X-ray energy of the 2011 outburst is $5.77 \times 10^{48}$~erg \citep{Miller:2014bs}. Averaging over the outburst decay time of 110 days, the average X-ray luminosity is $\bar{L}_{x}=6 \times 10^{41}$~erg/s. On average, a typical value of $\sim$10\% of the accretion power thought to go into to the jets during radio loud phases of accreting black holes \citep[e.g.][]{Falcke:1995yb}. Therefore, the expected average total jet power of HLX-1 is $\bar{Q}_{j}\simeq6\times10^{40}$~erg/s. This average jet power is somewhat lower than the estimate from a hard state compact jet, where \citet{Kording:2008nq} also assumed a 10\% jet efficiency, but consistent within the errors.

\subsubsection{Higher BH mass or an outlier on the fundamental plane?}

After applying the slim disk model of \citet{Kawaguchi:2003uq} to the X-ray spectra of HLX-1, \citet{Godet:2012ys} found a best fit BH mass of $M_{\rm{BH}}\sim2 \times 10^4$~M$_{\odot}$. Similarly, a more sophisticated modelling that employs a relativistic slim disk with full radiative transfer resulted in a mass of $M_{\rm{BH}}\simeq(0.6-19.2) \times 10^4$~M$_{\odot}$, depending on spin and inclination \citep{Straub:2014fk}. On the other hand, the chosen disk model does not affect significantly the BH mass estimate and if applying a standard disk model, the upper end of the mass of HLX-1 was found to be $3\times10^5$~M$_{\odot}$ at 90\% confidence \citep{Davis:2011oq}. On the contrary, the BH mass obtained from the fundamental plane is at least a factor of 10 higher than obtained from the X-ray spectral fits and it is not consistent within the 90 \% errors.

In the model of \citet{Godet:2012ys}, the peak accretion rate is $\dot{M}=4 \times10^{-4}$~M$_{\odot}$/yr and during a hard state it is $\dot{M}<4 \times10^{-6}$~M$_{\odot}$/yr. Also, \citet{Straub:2014fk} found an accretion rate of $\dot{M}=(0.3-2) \times10^{-4}$~M$_{\odot}$/yr during burst. The mass accretion rate deduced assuming the presence of a compact jet is also at least an order of magnitude higher than the accretion rate derived from X-ray spectra and the estimates are not consistent within the errors.

Furthermore, the star cluster that hosts HLX-1, has an inferred mass of $10^5-10^6$~M$_{\odot}$ \citep{Farrell:2014cr} and to have a BH mass to cluster mass ratio in the order of unity is unlikely \citep[e.g.][]{Miller:2002rq}, however, recent results show that in compact dwarf galaxies the ratio could be as high as 15\% \citep{Seth:2014vn}. We assume that the correct BH mass is estimated from the X-ray spectral fits. The resulting high BH mass (and accretion rate) obtained from the fundamental plane could then indicate that HLX-1 is an outlier source. It is either radio bright or X-ray faint with respect to the correlation. A comprehensive study of a sample of such outliers \citep{de-Gasperin:2011uq} concluded that those sources are X-ray faint rather than radio bright. On the other hand, in the case of HLX-1, the hard state X-ray luminosity is only a factor of $\sim100$ lower than the peak X-ray luminosity and therefore we argue that HLX-1 is rather radio bright. So, the radio emission could be Doppler-boosted and the above estimates should then be considered as upper limits.

\citet{Miller-Jones:2006uq} argues that an unconfined, hard state compact jet may have a Lorentz-factor above $\Gamma\simeq2$. The Lorentz-factor is $\Gamma = (1-\beta^{2})^{-0.5}$, where $\beta$ is in units of speed of light and the Doppler-factor is $\delta=\left[\Gamma(1-\beta \cos \phi)\right]^{-1}$, where $\phi$ is the viewing angle. The Doppler enhancement is proportional to $\delta^{3-\alpha}$ and it has a maximum at $\delta_{max}\simeq2\Gamma$. Here, we conservatively assume that our compact jet has a $\Gamma=1.4-2$. Then, the radio emission could be boosted by a factor of up to $22-64$ for a flat-spectrum jet\footnote{Applying this value to the radio emission and using the fundamental plane would still give a mass estimate consistent with the X-ray spectral fits.}. To have a consistent mass estimate from the fundamental plane, the radio emission of the compact jet has to be boosted by at least a factor of $\sim5$, which would limit the viewing angle to $\theta \leq 34^{\circ}$ (to the angle where $\delta^3 \geq 5$). On the other hand, in Sec. \ref{fl}, based on the energetics we argue that the flares may not be boosted or could even be deboosted at the same time. This could be the case for certain viewing angles if the jet has a higher Lorentz-factor during a flaring event. Assuming a maximum of $\Gamma=10$ for a flare would limit the viewing angle to $\theta \geq 25^{\circ}$ (the angle where $\delta\leq1$). Therefore the case of a mildly boosted compact jet and a deboosted flare is possible for a viewing angle range of $\theta \simeq 25^{\circ} - 34^{\circ}$, which would also limit the minimum Lorentz-factor of the flare to $\Gamma=5.5$, assuming identical viewing angles for the compact jet and the flare. In this scenario the maximum Doppler enhancement would be 7.4-12.3 for the compact jet.

Alternatively, a face-on SS433 type system has been proposed for some ULXs \citep{Fabrika:2001fk} and recently specifically for HLX-1 \citep{King:2014uq}, who argue that the geometric beam cone (or ' funnel') has an opening angle of $1.6^{\circ}$. This is a tempting geometric model to apply to our radio observations. Taking a distance of 5.5~kpc and an integrated flux density of S=0.7 Jy for SS433 \citep[e.g.][and references therein]{Miller-Jones:2008uq}, the source would have an integrated flux density of 2.3~nJy if placed at the distance of HLX-1. To match the measured flux density of HLX-1, a Doppler enhancement of at least $\sim$9400 (or $\delta \geq 21.1$) would be required. Assuming that the radio jet has a viewing angle similar to the quoted geometric beam opening angle (i.e. it fits into the funnel), a Lorentz-factor of $\Gamma \geq 12$ would be required. This would mean a highly relativistic jet (0.996~c) that might be in contrast to SS433 whose jet is likely to be mass-loaded and has a speed of only 0.26~c. In any case, this geometric model could be applied to the radio emission, albeit, this model does not explain the X-ray spectra and state transitions of HLX-1 \citep{King:2014uq}.

\subsection{Flare properties of HLX-1}\label{fl}

In this Section, we investigate the energetics and kinematics of the radio flares detected in 2010 and 2011 and discuss the possibility that the radio emission detected in 2012 is not related to the X-ray hard state.

\subsubsection{Flaring behaviour}

We observed HLX-1 during its outburst with the VLA to catch flares and to study their time evolution. However, we did not detect new flares in our 2012 campaign. With respect to the deepest VLA noise level, we find that the previously detected flares are variable by a factor of ten. Also, the apparent variation of the spectral indices ($\alpha_1,\alpha_2,\alpha_3$) is consistent with a variable jet source. This is because $\alpha_3$ indicates an inverted radio spectrum that is peaking in the 9-GHz band (or higher). Within the errors, it may be more inverted than allowed by a synchrotron self-absorbed core of a conical jet of $\sim1.5$ \citep[e.g.][]{Paragi:2013kx}, that may indicate a flare or discrete ejection. Inverted spectra are typically seen in synchrotron self-absorbed objects, where the signature of the evolution (or age) of an ejection is that the synchrotron turnover frequency shifts from high to low frequencies with time due to the expansion and the radiative losses of the ejected material. However, the exact dynamical evolution of a flare will depend on the ejected mass, on its initial Lorentz-factor, and ISM density \citep[e.g.][]{Peer:2012fk}. There are example radio spectra of flaring microquasars, like GRS1915+105, that show a turnover frequency at $\sim1-3$~GHz \citep{Rodriguez:1995kx}. In the case of Cyg X-3, the turnover is at $\sim7-10$~GHz  \citep[e.g.][]{Marti:1992vn}. This kind of radio spectrum is also exhibited by AGN flares, where the actual shift of the turnover frequency may start from 10s-100s of GHz and could be tracked by having several broadband radio spectra measured, that is allowed by a much longer flaring timescale \citep[e.g.][]{Hovatta:2008fk}. In this regard, HLX-1 exhibits radio properties that are typical for flares in jets that also complies with the interpretation of the radio emission being due to flares \citep{Webb:2012kx}.

Furthermore, the X-ray evolution of HLX-1 shows state transitions \citep{Servillat:2011fd,Godet:2012ys} similar to microquasars \citep[e.g.][]{McClintock:2006fv,Fender:2009bh} and radio emission was detected following these transitions \citep{Webb:2012kx}. These flares are thought to occur after crossing the ``jet line" \citep{Fender:2009bh} on the hardness-intensity diagram of the outbursts, still, it is not straightforward to estimate an exact arrival time. In HLX-1 radio flares were detected after reaching the X-ray peak (Fig \ref{lc}), when the source was already in a disk dominated state, where the radio emission is quenched in most cases of microquasars. On the other hand, as observations show, flares can indeed occur during a purely disk dominated state and some sources do not seem to completely quench in radio \citep{Brocksopp:2002cr,Brocksopp:2007fk,Brocksopp:2013uq}. Nevertheless, in some cases it is also common to have a major flare that is later followed by multiple smaller ones, see e.g. Fig. 4 of \citet{Brocksopp:2002cr}. \citet{Webb:2012kx} showed a detection of at least two flares from HLX-1 in 2011, that may indicate similar flaring activity in HLX-1. However, \citet{Brocksopp:2013uq} have shown that the different subsequent flares have diverse spectra, duration, and morphology, which could be due to multiple ejecta or due to rebrightening. This is because instead of a simple flux decay, as a result of a ballistic motion, the rebrightening may reflect an additional deceleration due to the interaction with an earlier ejecta or with the ISM.

Here, we account for the possibility that the radio emission detected in 2012 is not connected causally to the X-ray state, rather to the flaring activity. In this case, one has to explain a variable source, as argued in Sec. \ref{bubble}, that slowly decelerates. The average flux density of the flares in 2011 was about 45~$\mu$Jy, that then dropped to $\sim22$~$\mu$Jy within $9-11$~months, considering the detections in 2012 May and Aug. This hard state flux density then dropped below 6.3~$\mu$Jy in 1 month, when the first VLA observations were carried out. In principle, such a slow deceleration might not be excluded as some microquasars show ejecta interaction with the ISM on timescales up to years  \citep{Corbel:2002qf} and we would not be able to spatially resolve such components at the distance of HLX-1. On the other hand, the number of measurements are not sufficient to model a decay time. Still, we posit that a simple exponential flux decay is unlikely on the above timescales. This is because the flare emission detected in 2011 has already varied within a few days \citep{Webb:2012kx}, that may indicate a more rapid cooling. Also, we could easily miss flares in 2012 due to a potentially short flaring timescale, i.e. due to sparse sampling or bad timing, given that the VLA on-source time is limited to 1 hr, while the ATCA integration times were much longer on the order of 7-9 hr. If the flares are variable on the order of a day or shorter, then one has a much lower chance to catch a flare with the VLA.

Flares are typically a factor of 10-100 above a non-flaring continuum \citep{Brocksopp:2002cr,Brocksopp:2013uq} and our $3\sigma$ limit of 6.3~$\mu$Jy may imply that in HLX-1 such continuum level is below this limit or the source does quench between the subsequent flares. Based on this, a compact jet would be expected to have a much lower flux density than the flares, lower than the measured factor of 2-3. Given the relatively short variability timescale and the apparently high flux density with respect to the flares, one may also conclude that the radio emission is boosted. Alternatively, we missed the major flare, which may involve the future possibility of detecting flares closer to mJy levels.

\subsubsection{Energetics and beaming}

In the following we assume equipartition and estimate a minimum jet power ($Q_{min}$) of a single associated ejection event corresponding to the highest flux density on 2011 Aug 31 to compare with our average jet power
deduced in Sec. \ref{jet}. This can be estimated from the following equation \citep[e.g.][]{Longair:1994hs,Miller-Jones:2006uq}, that we parametrized for HLX-1:

\begin{equation}
\begin{split}
Q_{min}=4.67 \times 10^{36} \eta^{4/7} & \left( \frac{t_r}{\rm{day}} \right)^{2/7}  \left( \frac{d}{\rm{Mpc}} \right)^{8/7}  \left( \frac{\nu}{\rm{GHz}} \right)^{2/7} \\
 \times & \left( \frac{S_{\nu}}{\rm{\mu Jy}} \right)^{4/7} \, \rm{erg/s},
\end{split}
\end{equation}
where $\eta-1$ is the ratio of relativistic proton to electron energy, $\nu$ is the observing frequency, $S_{\nu}$ is the observed flux density, $d$ is distance, and $t_r$ is the rise time of the flare. This equation does not account for a kinetic energy associated with the bulk motion of an $e^{\pm}$ plasma (nor of an $e-p$ plasma). Also, in the above equation the volume of the ejecta is derived from its light crossing time, which is approximated by the rise time of the flare. We do not account for relativistic protons ($\eta=1$) and use a flux density of $\sim$63~$\mu$Jy at 7~GHz central frequency. The rise time is not known, however, based on the variability seen in the 2011 observations \citep{Webb:2012kx}, we assume a fiducial value on the order of a day and we provide $Q_{min}$ as a function of this parameter:

\begin{equation}\label{obsframe}
Q_{min}=1.6 \times 10^{40} \left( \frac{t_r}{\rm{day}} \right)^{2/7} \, \rm{erg/s}.
\end{equation}

$Q_{min}$ is not a strong function of the rise time and the uncertainty in our estimate could be dominated by the unknown beaming effects. Such beaming effects are necessary to invoke because the hard state jet power is a factor 10 higher than the jet power of the brightest flare, if taken at face value. So, either the compact jet is boosted or the flares are deboosted. In the following, we investigate the possible intrinsic power of an apparently deboosted flare.

To have an insight into the intrinsic jet power, the derived $Q_{min}$ has to be transformed to the rest-frame by scaling it by a factor\footnote{Note that this correction factor is model dependent as the emitting volume is estimated from the rise time that also suffers time dilation. For instance, if the volume can be estimated directly from high-resolution observations, then the correction factor needs to be modified accordingly.} of $\delta^{-(3-\alpha)4/7}$  \citep[e.g.][]{Miller-Jones:2006uq}, where $\delta$ is the Doppler-factor. To estimate the correction factor, we consider a deboosted approaching jet -- neglecting a receding jet -- and an acceptable range of $\Gamma\simeq[1.4;10]$. The lower end of this range reflects one of the lowest $\Gamma$ measured among microquasar ejecta \citep{Yang:2011fk}. While, the upper end was chosen to account for a possibly high $\Gamma$, should the ejecta have not been frustrated \citep{Miller-Jones:2006uq}. Given the unknown viewing angle, this range of Lorentz-factors translates to a minimum and maximum $\delta$ of $[0.1; 20]$. Then, a correction factor of up to 193 could be obtained for $\alpha=-1$. Therefore, a deboosted flare might not be excluded. However, as argued in Sec. \ref{jet}, it is unlikely that the intrinsic jet power of an ejection is larger than the overall average output and the boosted compact jet scenario is favoured.

\section{Conclusions}

We investigated the radio properties of HLX-1 using a set of follow-up ATCA and VLA observations. These involved observations during a hard X-ray state (ATCA) as well as at the beginning and during the decay of the 2012 outburst (VLA). We detected radio emission at the location of HLX-1 when the source was in a hard state. Under the assumption that the emission is coming from a compact jet we provide an independent mass estimate of the BH of $M_{\rm{BH}}\leq2.8^{+7.5}_{-2.1} \times 10^{6}$~M$_{\odot}$ at 90\% confidence. We also investigated the possibility that this radio emission could be due to a radio nebulae, star formation, a residual of the flaring activity. We conclude that the detected emission is not compatible with a nebula or star formation and it is unlikely to be due to a jet interacting with the ISM, because the variability seen on much shorter timescales. We argue that the radio emission is likely to be Doppler-boosted making the mass (and accretion rate) estimate an upper limit. The follow-up VLA observations do not reveal new detections, possibly due to an insufficient sampling of a relatively short rise time of the flares. The VLA data suggests a variable radio source and the flare energetics, based on analogies with microquasars, also suggests a boosted radio source. Further radio monitoring is needed to test the time-dependent behaviour and the compactness of the radio emission, perhaps with the MeerKAT or the SKA.

\section*{Acknowledgments}
We thank the anonymous referee for the quality comments that improved the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Australia Telescope is funded by the Commonwealth of Australia for operation as a national facility managed by CSIRO. The authors are grateful to N. Gehrels for supporting {\it Swift} observations of HLX-1. This work made use of data supplied by the UK {\it Swift} Science Data Centre at the University of Leicester. EK acknowledges fund from an NWO Vidi grant Nr. 2013/15390/EW. SAF was the recipient of an Australian Research
Council Postdoctoral Fellowship, funded by grant DP110102889. The Centre for All-sky Astrophysics (CAASTRO) is an Australian Research Council Centre of Excellence, funded by grant CE110001020.

\bibliographystyle{mn2e}

{\small

redpajama_set_name: RedPajamaArXiv


text:
Open main lifestyle navigation Lifestyle
trending now in Lifestyle
Surgeons extract condom-wrapped banana man ate in 'hormonal...
Wife attacks Thai sex worker she found having sex with her husband
My Central Park proposal went viral — I was horrified by the...
Starbucks customer slammed for $2 tip refund request: 'I would...
I got an upside-down pineapple tattoo — I didn't know its racy...
I grew up in a cult with my dad, 5 moms and 44 siblings — I...
AI technology could make these jobs obsolete: 'The wolf is at the...
Why more women, like me, are abandoning the birth control pill...
'Friends' pop-up shop in NYC for 25th anniversary: How to get tickets
Michael Starr
Social Links for Michael Starr
Matthew Perry, Jennifer Aniston, David Schwimmer, Courteney Cox, Matt LeBlanc and Lisa Kudrow in "Friends." Warner Bros. Productions
More On: pop-up stores
Gelt-y pleasure: Pop-up Hanukkah bar coming to NYC
Apartment Therapy launches shoppable pop-up for small spaces in Soho
Amazon to close 4-star shops, bookstores to focus on Whole Foods, Fresh
'Bowie 75' pop-up shops in NYC and London honor David Bowie's legacy
Call it "The One with The Pop-Up."
Warner Bros. TV has dropped new details about its "Friends" pop-up experience being staged in conjunction with the classic NBC sitcom's 25th anniversary.
The nostalgia-packed, month-long pop-up will be based in two places in SoHo from Sept. 7 to Oct. 6, with the ticket-holder entrance located at 76 Mercer Street (between Spring and Broome) and a retail store entrance at 503 Broadway.
The store will be open seven days a week, from 10 a.m. to 10 p.m.; tickets to visit the pop-up are priced at $29.50 a pop and will be available starting Friday. Aug. 2 online at Friends25popup.com.
The space will offer set re-creations, as well as props and costumes that were used on the series, which was set in New York City and aired 236 episodes from 1994 to 2004. The show made household names of Jennifer Aniston, David Schwimmer, Lisa Kudrow, Matt LeBlanc, Courteney Cox and Matthew Perry — and spawned the short-lived spinoff "Joey," starring LeBlanc reprising his doofus "Friends" character Joey Tribbiani.
Fans will be able to "peek through Rachel and Monica's purple door, relax on Chandler and Joey's recliner after playing some foosball, or help Ross with the infamous sofa pivot," according to a Warner Bros. press release touting the pop-up, which is sponsored by Superfly, Warner Bros. Consumer Products and Warner Bros. Television Group.
The pop-up's first day, Sept. 7, will be open only to AT&T customers via the AT&T Thanks app.
pop-up stores
Read Next Woman shouts 'shame on you' in homophobic rant at Pride ma...
This story has been shared 126,901 times. 126,901


text:
Q: Big O Notation Exercise I'm having a small problem. I'm very new in this section so please bear with me.
I understand Big O meaning what everything signifies like the $O(n), O(n^2), O(x^n), O(\log n)$ and $O(1)$.
I also learn the very basic of $\Omega$ and $\Theta$.
The problem that I have is I'm being as to represent this as a theta:
$T(n) = 2n+\log^2n$
I am not sure what the answer is i just assumed it was $\Theta(n)$ because we're talking about worst case algorithm.
Am I correct ?

A: Yes, $2n+\log^2n$ is $\Theta(n)$, but not because you are talking about algorithms, worst case or otherwise. $2n+\log^2n$ is $\Theta(n)$ because there are constants $k_1$ and $k_2$ such that, for large $n$, $$k_1n\le2n+\log^2n\le k_2n$$


text:
2019: A forward-looking retrospective
Author: Joseph Clark
Douglas Max Utter, "Ratman." Spray
paint and latex paint on Arches, 65" X 45", 1986
Elsewhere on the digital pages of CAN, Brittany M. Hudak and Michael Gill have written fine-grained and big-picture analyses of the year in Northeast Ohio art. Hudak remembered the year in a series of particular exhibits; Gill contextualized local developments within larger trends in the artworld. This post, then, is calibrated towards the medium scale—events which made a great immediate impact, or which will influence the arc of the future.
2019 marked the 50th anniversary of MOCA Cleveland's founding, and its seventh year in its permanent home on Euclid Ave. The institution marked the occasion by eliminating general admission fees. Free admission fulfilled a longtime dream of Director Jill Snyder. It also let MOCA match the pace of its neighbor two blocks over, the Cleveland Museum of Art. Appropriately, this year CMA and MOCA undertook one of their most ambitious collaborations. The two museums co-hosted Invisible Cities, the first solo exhibition by Chinese artist Liu Wei. Wei's digital paintings and monumental sculptures offered viewers not only a glimpse into Chinese attitudes about the sprint toward a technological, city-dwelling society; but also the opportunity to pause and think about America's own urbanization.
Another anniversary was marked by Art House, Inc., which celebrated its 20th year. The Brooklyn Centre-based organization offers creative education to multicultural children who rarely see themselves reflected on museum walls, and adults of all ages and classes. For a victory lap, past and present Art House instructors displayed works at Studio 215.
Perhaps no other Northeast Ohio artist received—or deserved—as much recognition as Douglas Max Utter. The expressionist and CAN contributor was the guest of honor at ARTneo's 35th anniversary benefit, and subject of a career-spanning exhibit curated by himself and HEDGE Gallery proprietor Hilary Gent. Following publication delays, a catalogue and essay collection based on Falling from the Sky of Now is forthcoming in the new year. As a painter as much as a critic, Utter has been a central voice in Cleveland's artistic conversation for decades. He is more than deserving to be subject of that discussion.
Detail from Meng-Hsuan Wu's "Passage." Marbling paint and wood burning on basswood.
For a decade, FORUM Artspace was a fixture of 78th Street Studios. Many recent graduates found a friendly venue there, under the curatorship of Karl Anderson and Michael Abarca. Jan. 18, FORUM's final exhibit in its Ohio City home—aptly titled Into the Sunset—closed. Anderson and Abarca said that they remained open to curating future projects under FORUM's banner. However, a permanent brick-and-mortar home for FORUM is not on the horizon. It will be missed, both for its particular character, and out of a general longing for spaces which invite early-career artists.
Earlier this month, Photocentric opened its first Hopeful exhibit at Waterloo and E. 156th . Michael Loderstedt's new gallery will display contemporary photography, in all its permutations. Hopeful features a diverse range of photographic practices, including Nancy McEntee's haunting, mysterious portraits of her daughter; Lori Kella's images of ecologically-minded dioramas; and Bruce Checefsky's time-lapsed garden photography, made with a scanner opened up to the daylight.
In March, RANT! Gallery held its inaugural exhibition, reuniting a stable of artists cultivated by Dan Miller during his years at Rotten Meat Gallery. Six years elapsed between Rotten Meat's closing and RANT's debut. But in that intervening time, Miller maintained and enlarged the trust he had earned from the Cleveland creative community. His new gallery maintains the freshness, wit, and resourcefulness which characterized Miller's past curations.
(We would be remiss not to mention an even more personal accomplishment of Miller's. In partnership with the Maria Neil Art Project, Miller exhibited Some Disassembly Required. This painting series functioned as a sort of visual memoir, recounting a few harrowing years of Miller's life with mental illness. Their emotion and raw honesty are both a triumph and a service: an invitation to break stigma, ask for help, and bring private struggles into public.)
Portrait of Tamir Rice by Antwoine Washington
In November, Samaria Rice announced several initiatives aimed at empowering children of color through play, creativity, and culturally competent education. As reported in CAN, Rice will partner with the Cleveland Foundation to fund projects serving the city's youth. She will also oversee the foundation of the Tamir Rice Afrocentric Cultural Center, a planned "safe, accessible and inspirational space" for youth on the West Side.
For this critic, the most consistently impressive and surprising curator in 2019 was Anna Tararova. Tararova works as Gallery and Artist Opportunities Coordinator at The Morgan Conservatory. This year, she organized No More Tears at Survival Kit Gallery and Printmaking as Resistance: Exhibition + Zine Library at the Morgan. Tararova had curated prior to 2019, but these two shows commanded attention. Both exhibits deftly integrated art objects from radically different media into singular, seamless experiences.
No More Tears explored experiences which are almost universal, but rarely discussed. Paintings by Nikki Woods and Lauren McKenzie depicted the stress and strain women are expected to hide from view. Zak Smoker's striking installations explored the corruption of childhood by such forces as bureaucratized education and normalized media violence. All the objects in the show were striking, but each artist cultivated their own themes and moods. There was a real danger that these bold works might shout over each other—but Tararova gave each the space it needed to have its say.
A planning sketch for Zak Smoker's "The Chalkboard Is Not A Toy", printed in a zine by Ana Tararova.
Printmaking as Resistance was both an exhibit and a session of political education. The art objects on display did not merely express political sentiments, but were themselves embodiments of live political campaigns. Tararova assembled a broad selection of agitprop posters, educational flyers, and "zines" (limited-circulation magazines, monographs, or anthologies printed independently on a shoestring budget). These images were produced in service of such causes as anticapitalism, student movements, immigrant rights, prison organizing, and indigenous self-determination.
Printed matter has long been a powerful tool of protest and movement-building, especially on the radical left. This is especially true of zines, which have been especially favored by feminists and LGBT+ activists traditionally excluded from more mainstream outlets. Tararova elaborated on this historic context in an educational presentation during the show's run. For both aspiring activists and those simply curious about the leftmost reaches of the political spectrum, the Morgan show was a valuable seminar.
We will not single out a "favorite" individual painter for the year. However, we will name a tendency which repeatedly attracted and intrigued us. This tendency was not a movement, per se. We have no reason to think the artists we associate with it influenced each other, or drew inspiration from shared sources. However, they did converge on similar themes, methods, and images: vivid color palettes, abstract environments, and extreme closeups of pained expressions on human (sometimes humanoid) faces. Call the genre "neurotic portraiture." It was exemplified in Eric Rippert's The Man Whose Head Expanded at Bay Arts; Nikki Woods in the aforementioned No More Tears; and Emma Anderson in I/You/She at BOX Gallery.
Nikki Woods, "Smoking/Crying." Oil on canvas.
Recently, Rippert has shifted away from pure abstraction to stylized figures. But his characters are not all right. They have inky black eyes, or the hollow white faces of skulls. They stand for family photos, bored, stiff, or cruelly smirking. Empty sockets make eye contact with viewers, widening as if to beg for help. Woods' women slump under the weight of lumpy demons on their shoulders, or melt before our eyes. Anderson's totemic "alter-egos" speak with a hundred voices about self-doubt, fear of death, and the feelings of unraveling which come from being pulled from many directions.
Like the anatomical drawings of Renaissance polymaths, these painters collapse the "beautiful-grotesque" dichotomy. From a radically formalist perspective, one which only considers a painting as a two-dimensional pattern of colors and shapes, these images are beautiful. But when considered as pictures of things, representations of persons and objects outside themselves, they can be disturbing. Often, the disturbance is softened by humor. Woods excels at deadpan; she can make her subjects shrug with their eyes. Anderson and Rippert are almost cartoonists, using rubbery exaggeration and loud colors to heighten emotion. But all three painters are gallows humorists. They joke to express anxiety, exasperation, fear, exhaustion. Many of us feel just these things going into the election year 2020, and are lucky to have such able painters depicting them.
Emma Anderson, "Falling While In My Own Head." Acrylic on canvas.
tagged with Anna Tararova, Art House, ARTneo, Bay Arts, Box Gallery, CAN Blog, cleveland museum of art, CMA, Dan Miller, Douglas Max utter, Emma Anderson, eric rippert, Forum Artspace, HEDGE Gallery, Jill Snyder MOCA Cleveland, joseph clark, Maria Neil Art Project, Morgan Conservatory, Photocentric, Rant Gallery, Rotten Meat Gallery, Survival Kit
The opinions expressed on CAN Blog are those of the individual writers. Art is somewhat subjective. Well, somewhat. But yes, everybody's a critic.


An imaginary story book series, much like a parable, set in another time in another place. Keen readers will pick up on what it is saying beyond the story line. Others will simply enter the pleasant realm it paints, taking a refreshing break from their usually surroundings and challenges. Enjoyable, mysterious, promoting good character-building and encouraging happy communities and families. Maybe your community will wish to adopt some of the costumes of the land where Celtellina lives. Maybe you too will find the treasures as you take the secret journey, like she did. Aimed for older children and youth, on up, but content pleasant, so all ages may enjoy hearing it—though the older and wiser-minded ones will appreciate and grasp it more deeply.