Sourcing: Training a horse to pull a 1,000-pound carriage is a difficult and time-consuming process, with no guarantee that the horse will be up to the task. Since carriage drivers do not have the time, facilities, or funds to do this themselves, they purchase horses who are already accustomed to pulling a carriage. Such horses most often come from farms, where they have already put in many years of labor and are being sold because they are no longer capable of working on the farm. Once they become urban carriage horses, their lifespans are greatly reduced. A recent study, using New York Department of Health data, determined that the annual turnover of New York City carriage horses is over 30 percent (source: banhdc.org). Horses not re-registered are sold at the same auctions where they were purchased, either to return to farm work or be sold for slaughter, with only rare opportunities for true retirement.
Pollution: Carriage horses, particularly in heavily congested urban settings such as New York City and Chicago, spend much of their day breathing exhaust fumes from cars directly in front of them. Horses also spend hours walking through a miasma of oil, road salt, and other roadway pollutants. The health issues associated with chronic exposure to airborne and ground pollution—well-documented in people—affect horses, as well. Even when horses are not pulling carriages, they are kept in inadequately ventilated stalls where they are exposed to high levels of dust contaminated with mold and other fungi. Long-term exposures to these elements lead to many respiratory conditions, including bronchitis, rhinitis, inflammatory airway disease, and reactive airway disease.
Noise: In urban settings, carriage horses are exposed to near constant, high levels of noise—up to 100 times louder than a typical conversation (http://nymag.com/nymetro/urban/features/noise/9456/: often 80–100 dB). Chronic exposure to street noise—linked to hearing loss, poor cardiovascular health, and stress in people—most likely affects horses similarly. Further, sudden noises may frighten the horses, causing them to bolt, resulting in harm to themselves, the carriage passengers, or other vehicles or bystanders. Every year in New York City, there are multiple accidents involving carriage horses that have been startled by sudden noises.
Weather: Carriage horses are exposed to a wide range of temperatures and humidity levels. In New York City, the regulations allow for their use pulling carriages whenever the temperature is between 18 and 90 degrees Fahrenheit (in Chicago, the minimum allowable temperature is 15° F). There are no regulations regarding humidity. Road conditions at the edges of the temperature range can be a serious issue. In hot weather, asphalt temperatures may be 50–100° F higher than the air temperature and can damage the sensitive areas of the hoof. The extreme heat also puts the horses at risk of dehydration and overheating. A typical horse will drink 5–10 gallons of water a day. Horses pulling carriages in high heat require much greater volumes (15–20 gallons), as they may lose over 10 gallons of water from evaporation. This much water is difficult to provide in the urban setting, even when water troughs are available. During high humidity days, the horses may be unable to properly cool themselves through sweating or other measures, putting them at further risk of overheating.
While the dangers of dehydration and overheating are reduced in cold weather, there are still problems. For example, salt-treated roadways are the same temperature as the air and can cause frostbite to the hoof.
Urban carriage horses are purely a tourist attraction—not a necessity. Given the many documented health and welfare issues for the horses, the only sensible solution is to ban them from use. Legislation has recently been introduced in New York City to end horse-drawn carriage rides as of June 2016 (New York City Council: Int 0573-2014). This legislation provides job training for the approximately 300 carriage drivers who would be affected by the ban and would also require proof that the carriage horses would not be killed after they are retired. The legislation is currently being reviewed in committee, with an uncertain future. In February 2014, a similar ordinance was proposed in Chicago to end the horse-drawn carriage industry there and retire the 25 carriage horses in use at that time. The Chicago ordinance is still pending in city council, with no timetable for advancing. Other cities are reviewing legislation, but none have proposed bans.
AWI supports a ban on horse-drawn carriages used as tourist attractions in urban settings. The constant exposure to traffic, noise, and pollution; the long hours of standing and walking on hard surfaces; the hard labor under sometimes extreme weather conditions; and lack of pasture access are not consistent with the owner's responsibility to provide high-quality, long-term care for the horses. For more information about AWI's policy on horse welfare please follow this link: http://awionline.org/content/horses.


text:
QATSICPP Newsletter – January 2020 Edition
QATSICPP Newsletter – January 2020…
As we launch into 2020, I would like to acknowledge the dedication and commitment of our united sector and ask you to take some time to reflect on our collective achievements over the past year and more importantly over the last 10 years. The QATSICPP membership has risen to a remarkable 34 members across the state, we now employee 15 staff as we continue to be led by the voices of our children, young people, families and their communities to keep and grow our children safe, in family, community and culture. We will continue to provide leadership in advocacy, and the development of policies, strategies and programs to resource, support and strengthen the capacity and capability of Aboriginal and Torres Strait Islander Community Controlled Child Protection Agencies in the interests of our children, young people, families and communities.
Read the full newsletter
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The Queensland Aboriginal and Torres Strait Islander Child Protection Peak acknowledge the Traditional Custodians of the lands in which we work and honour the Elders, past, present and future.
QATSICPP are strong supporters of the Family Matters Campaign
Aboriginal and Torres Strait Islander people should be aware that this website may contain images, voices or names of deceased persons in photographs, film, audio recordings or printed material.

redpajama_set_name: RedPajamaCommonCrawl


text:
What do you think: A Preview of Stolen Warrior
by LeTeisha Newton | Jun 30, 2012 | Books | 0 comments
Everything must Begin
"There are times when I doubt the intelligence the Gods have given you Tuel. It is not healthy to ask all that you do. Mark what I say, that tongue of yours will land you in places not to your liking. Know you not the dangers you present? Can you not see what will happen to the like of you?" Vite let out a breath when she finished. "I vow you will be the death of me, beloved friend." She then gave Tuel a loving smile. "I state only what I know to be true. I do not want you to see harm." She placed a hand on Tuel's shoulder. "Here is not a place of forgiveness." Vite whispered. Her eyes seemed to glaze over as she looked into the past. She was remembering Lani.
"There is nothing your words could have done for her Vite." Tuel said consolingly. She knew what Vite was thinking of. Lani had been a beautiful woman; they always took the beautiful ones. In their later years Vite and Tuel had earned the respect of the Dome. They had lasted long in the world around them and had privileges because of it. She sighed; she did not miss the days when she battled. She feared the only reason for her and Vite's survival was because fewer women had stood in the way then. It was easier to defend oneself against ill-schooled chits. But now their battle days were over and their only reason for existence was for the training of the new women to come. Such a sad life they had in store.
"I know Tuel, but I was fond of her no less." Vite looked at seven girls sleeping soundly. They had no fear, as of yet. There was still another shipment to come with a head count of ten by five she was told. When they arrived the training would start, and then the hard life would begin. "I hate what we know these girls will soon do to each other."
"It is not something we can change. It never has been, my friend. This is their fate as it has always been." Vite said, sighing. "We will do what we must when they come and hope they survive."
"Very well Vite, very well." They sat in a comfortable silence for a time. Both were deep in their thoughts. What the next day held they did not wish to know. The world of the Dome was not a place for softness and many of these women would not last long. None would ever see their homes again. The sooner they accepted that the stronger they would be.
That had been Lani's mistake. She had always thought she would return home to her planet Foa and so she had not trained for her survival but merely to bide her time until a search party rescued her. It was when she realized the distance Cydria was from civilized worlds that she began to become careless. Tuel could not impart to Vite that Lani had been fighting in search of death. Home was where she wanted to be and the desertion of that notion depressed her. It was the last chink in her already failing armor. It did not take long before Lani, still achingly beautiful with her long flowing black hair and tanned skin was carried into the under-chamber where they slept, dead. Her death served as a cool reminder that the Dome was all that there was for these girls.
It had become their homes. Dolph, Xiau, Foa, Lixen, Tirth, and Mence. These planets had no bearing to the girls now. Another lesson they had better learn quickly. The Dome was death knocking at the door. It was all really a test to see who could keep the door closed the longest. These girls had not the option that Vite and she herself had had. Scarcity of women and the Dome's newness in itself were the reasons they had survived to become trainers. In the present day there was a replenishing supply of women and the warriors whom called Cydria home gave much to keep the Dome alive and prosperous. It was Cydria's main profit and the Cydrians were not fond of the idea of losing it.
What disturbed Tuel the most though was the fact that a woman stood at the top of it all. Every battler of the Dome knew the face of Phera Lithe Mire. She oversaw battles along with the men of Cydria. She gloated at the stupidity of the women she had captured and basked in their deaths. Phera Lithe had a cruel beauty that was stark. Her coldness and fondness for pain had twisted her features into an almost unbearable beauty to rest eyes upon. But the men of Cydria loved her and found her unfailingly magnificent. They vied for her attention. It was their want to be her consort. What man would not want a woman of such pale, ethereal looks and turquoise eyes that seem to reflect all and see nothing? Any man would feel fulfilled by her side. She had not taken one as of yet but it was known that it was soon to come. There had to be an heir to take her place when she would leave. A cruel and just a coldly beautiful girl-child to follow in her mother's footsteps. It sickened Tuel. At the age of ten by four she was an old woman compared to the young ages of women who were being chosen to fight. They seemed to get younger and younger.
Tuel sighed. She knew why their age was growing younger. Phera Lithe wanted highly trained girls to watch. In this way the battles lasted longer, girls survived for longer and she had more money. Some girls who showed exceptional promised where pulled from the Dome and forced to be warrior concubines or, worst yet, chosen to be in Phera Lithe's army. She only chose the girls that had become bitter over their time in the Dome. She showed them false love and housed them in luxurious homes. They grew to love her and protected her blindly. Tuel knew it was not always out of pure compassion but the threat of being returned to the Dome. No one wanted back in after leaving and they knew if they returned their death would be forthcoming.
Yes, Vite and Tuel both were saddened by what the faceless unknown girls would have to face in this world. This world where men held the title warrior and boasted their prowess, but where women, with no title, except for amongst themselves, proved their prowess and were the real warriors.
The life to come for the seven and ten by five women was harsh. She only expected for twenty of the women to last to the next shipment. That was only a one-year away. A year of training and a year of battle. As they trained the shipment before them was using their skills to survive. When the new shipment came in another year Tuel's new women would begin to fight. It was an ever-going cycle. The Dome was never free of fights.
Some women bested their year of combat and were chosen to leave and lead other lives while others stayed and died off after another year or two. The way of the Dome was a short life span. The best way for a girl to live now was to last a year and hope to become a concubine or a foot in Phera Lithe's army. Tuel hoped for more women to be concubines then in the army. She could not stomach them defending a woman who had sent so many to certain death. It was left to be seen. Tuel stood slowly, smiling slightly at her soar joints. It was good to be alive. She had survived the Dome; it was all she could hope for. The seven that had already survived one year had just a short time to try to get into the Phera's good graces before they too would have only death.
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Kitchen and pantry door, with coat room at far left.
Countertop and right side of kitchen.
Hallway and room entrance. Home office is next door down the hall.
Entertainment center and patio door. Dining table is seldom used.
This is my home. It's on the ground floor in an apartment complex at the end of a cul-de-sac, on a hill adjacent to Route 89. It's very quiet compared to Oak Bay Avenue in Victoria, except for occasional carpet races by the Tang-fed toddlers upstairs. Most tenants are professionals or semi-professional students at the nearby Dartmouth-Hitchcock Medical Center. There is one California, two Oregon, one Florida, one British Columbia (mine), one Massachussetts, and two (upstate) New York license plates in the parking lot.
The sofa faces directly west, so I get plenty of sun in the summer. I really like the roomy kitchen, especially the counter-top. The long wall was immediately reserved for the 12' sailboard, leaving few options for the rest of the furnishings. Until yesterday (10/9/99), the dining table was up against the long wall, straddling the sailboard and leaving the two end chairs sticking out into the walkway behind the sofa. The only oddball item now is a long folding table that I've left in the kitchen, which I plan to replace. I could also use a bigger TV, but that can wait.
I didn't take any pictures of the two bedrooms, as I don't have a wide-angle lens. They are average size; not too big, but not small either. The far room is used as my home office. Both rooms can get quite warm from the sun. The bathroom is to the right of the kitchen. It's rather small, and lacks useful storage.
My prized possessions are kept indoors, while the rest are secured on the "deck". There's plenty of interior storage for my shop tools and supplies. Some of the kitchen cabinets are mostly empty. The coat room has more sports equipment than coats. Posters are VW and cycling promotional literature. More than good enough to call home.


Want to follow the U of Texas Conference on the Euro Crisis and the Modest Proposal?
Are you suggesting to face the truth to the eyes !!!??!!!
No Sir , prefer to watch the crucial political developments taking place in Greece right now !
Damn, and I have to work today!! I wonder if portions will be available for later viewing.
In Greece , there is a pandemonium so that Papandrew resigns !
Then , everybody would sign with their feet and teeth and hands the new loan agreement!
The whole parliament would sign it (constitutional condition ) and then every MP irrespectively of political side would congratulate each other . It would be celebrated as the Greece was rescued once more !
Could you have imagined this scenario one week ago ?
THIS IS CALLED SHOCK AND AWE gentlemen !
I guess i am a conspiracy theory enthusiast !
Great talk and discussion, we really need to hear that many times and study it. Excellent questions too. Hope you will upload this soon!
1) You stress the stand-alone nature of bonds which the ECB would issue (i. e. no guarantees from national governments). Please clarify for me: the national governments – through their NCBs – are liable for the ECB as far as I know. In other words, the ECB can't go bankrupt because the national governments – via their NCBs – would have to replenish the ECB's capital. So it is not a direct guarantee which would go into the national accounts but an indirect one which is just as good. Am I wrong?
2) As far as I can tell, we already have Eurobonds. When the ECB buys, say, Greek bonds and national governments are in the final analysis on the hook for the ECB, those bonds are now Eurobonds. Am I wrong?
3) From my dealings with the EIB over the years, I am afraid you overstate their potential role for a country like Greece (even if there were no co-financing required). The mindset of the EIB is "large projects" and not "middle-market projects". I am not saying that the EIB could not play a role in investments in Greece but they would be the larger investments. Given the structure of the Greek economy, a few large infrastructure projects may well fit in but that is unlikely to do all that much for domestic economic growth because large infrastructure projects are typically heavily foreign-sourced.
4) Thus, I believe what Greece needs is tons of middle-market investments (5 to at the most 500 employees) where you are only talking about single-digit EUR million numbers for individual investments (more likely in the lower single-digit numbers).
5) I am a firm believer that the true test if something works or not is if private capital can be motivated to flow. You sort of leave the topic of private capital on the side (perhaps thinking, correctly, that today only a fool would invest his private capital in Greece).
6) There is plenty of private capital available which would flow to Greece if the investors had the right security, competitive business framework and return potential. I am thinking of the hundreds of billion EUR which Greeks have in foreign accounts.
7) The security aspect can be taken care of by having the EU guarantee an Investment Law which Greece offers to those foreign investors.
8) The competitive business framework and return potential can be taken care of by establishing areas in Greece (I call them Free Trade Zones) where investors are offered everything they desire. I guess at the start it would be enough to have one in the Athens area and another one in the Thessaloniki area because this is where the population and the unemployed are. Someone has criticized that these FTZs would be "sweat-shops". I disagree. Many of the consumption products which Greece presently imports from, say, Central Europe are produced there and there are no "sweat-shops" in, say, Germany.
9) There are zillions of ideas floating around these days what "new-idea-projects" Greece could undertake (solar energy, etc.). In the longer-term yes; in the immediate short-term no, because those are untested areas and untested areas take time (which Greece presently does not have).
10) What Greece could do immediately is to start new middle-market businesses for the substitution of imported products which could just as well be produced in Greece if the security, economic framework and return potential were right. A little "infant-industry-protection" (import taxes) wouldn't hurt. I know this would violate EU-treaties but this, in my mind, cannot be a hindrance in times of emergency.
11) If Greece substitutes imports, the present exporters to Greece will suffer. That, however, could motivate them to shift some of their production to Greece so that you would not only have the offshore capital of Greeks as a source of foreign investment but also these foreign companies.
12) To sum up my point: Greece will have to reduce imports (i. e. standard of living) one way or another if foreign money no longer flows as in the past. If this reduction is not compensated by new domestic production, the Greek consumer will suffer badly. If it is substituted, the Greek consumer could perhaps hold on to his consumption habits but, at the same time, new domestic growth would be stimulated with new jobs, new incomes taxes and new corporate taxes.
Careful Yani. You may be close to some real animals.
I found the link below quite amusing and accurare, I hope you enjoy it too.
SYSTEM OVERLOAD – Feeling dizzy lately?
Phew, what a week, what a month, what a year….! The last week is a good example for chaos at work, or what is perceived as chaotic I should really say.
In reality, it is anything but chaotic, it is a reflection of massive social-political changes that are presented to the public on the grand stage as chaotic. Take this ridiculous stage managed G20 theater where besides the Merkozy's of this world, the finance ministers and central bank governors, Bill Gates is present as well, of course!
If you look at the history of achievements of this club, pretending to be an epistemic community, you will find nothing, exactly nothing but very high costs for security and wine and dine, the 2010 Toronto Bill came in at around 1,2 billion for the few days of their meeting there.
What should be a G-196 instead is a representation of the strongest, it is not a representation of the countries in this globalized world, and as such is equally an expression of post colonial elite mindsets at work. When talking about the G20 you have to talk about the IMF and World Bank at the same time.
When G-Pap announced his Referendum, I knew in the very same moment that this is nothing but political trickery, and that it would never take place. It simply can't be allowed by the powers at work behind the political stage, and they would do whatever it takes to prohibit this referendum, and I mean everything…..!
Democratic Lip-Services filled the news channels of most European countries. George Papandreou announced a referendum to be called to decide on the next debt deal that is forced upon Greece, and everyone in Europe was keen to express the democratic right of the people to vote on these decisions, decisions that determine their future and that concern them all, but in reality, somewhere in a room in Greece, the curtains are closed, no light can be seen from the outside, and a Barrett M95 had already a cold and polished .50 in it's chamber, just in case.
The next morning, and all the news papers were filled with one picture, and one picture only. The corps of G-Pap, headlines speculating who shot him, articles flooding the internet with theories, and on the political stage an international outcry would fill the news channels, followed by a ceremony of his burial and speeches to honor his legacy as a great politician, good friend, an outstanding Statesman, pillar of the Greek society, most important contributor to the European idea, and it should remain a talking point for years to come, just like JFK, but the politicos and media move on quickly, and the truth would never see the light of the day.
Somewhere on the caymans, a bank account filled up rapidly with substantial amounts. In Geneva in a private vault Gold bars are stapled for it's new owner, when a chap that looks rather like a first grade school teacher than a professional assassin, checks in at Athens airport. The thick glasses and his high pitched voice irritate the officer who is checking this Finnish passport, a first class replica that only very few people can get their hands on, when someone behind Dr. Aarne Rehn starts muttering about the efficiency of Greek services, armed with his two little obnoxious children left and right acting the Mickey he stares at the officer who is in the last 15 minutes of his long shift and then hands Dr. Aarne Rehn his passport nodding him through….
Ok, you are right, I admit it, I always wanted to write a political-thriller, and I do not know where this hotel room was, except that it is in a radius of no more than 2,0 kilometers to the target, who would not see it coming, a painless death, lights out, that's it, – grins -, but seriously now, would I be astonished if an assassination would have happened as a last resort to get rid of this referendum?
Nope, not a bit, it would not even trigger an eyebrow anymore!
So much is at stake for the players in this social engineering event that they would not hesitate to clear the path by all means possible, I have no doubts about this at all. A government politician from Finland was already publicly demanding tanks on the streets in Athens three weeks ago.
It is bad advise to focus on Europe exclusively these days when observing the developments that change the world.
UNESCO voted for Palestine membership, and it triggered a quick succession of events, Israel's increase of settlement policies, followed by the usual international diplomatic disapproval, a test launch of a nuclear capable rocket able to reach Iran, a headline about pre emptive strike possibilities, and a British announcement to stand ready should the US plan to intervene in Iran.
I think the Gaza peace flotilla is about to come closer today. Gaza has been under siege for more than 20 years now, depriving more than 1.5 million people of basic human rights, and it is essentially an American financed occupation, and their motivation and double talk is written all over the history of the Middle East.
I fully understand people to feel totally overwhelmed when faced with the flood of Informations that comes down the pipe these days. It is a lot to digest, and it is happening so very fast, but it always happens fast when big changes are about to occur.
We witness a change of global power dynamics, new emerging forces claim their stakes, old forces resist changes, and in between billions of people, confused, angry, scared.
People in Kenya saw the prices for their basic food double in a months, in Kibera one of the better know Kenyan slums, people can not afford the same amount of beens and bread like they could a week ago, traders behind solid iron bars, the Illusion of protection, hand over basic food for money from the spare shelves with very little goods.
Food prices, and commodities are just one aspect of the rigged markets, rigged by powerful speculators and the leaches on their arse who make a profit with death and starvation, it is nothing new, it is going on since decades. Joseph Ackermann took the stage and spoke of ethical markets, of deals not worth taking when they are unethical, right. Hitler warning the people on the dangers of fascism. Surreal.
The system's weakest points are uncovered, economical and political weak points, and people begin to understand a little better what goes wrong, but these are informed people, people who stay on the ball and developed critical analytic skills to be able to judge the events unfolding.
Make no mistake, most people are ill informed, brainwashed with daily propaganda, steered to react, steered to blame and steered to maintain status quo, to ridicule and marginalize those who question it, they are a majority.
Slowly people are waking up, the OWS like movements around the world are an expression of this awakening, they are not the majority of mainstream thinking, but they are right to point to the fact that they represent the 99% for other reasons.
Last week yet another young man in his 30's took his own life. I am always left speechless when I hear it, life is most precious, it is all that really counts. He was one of the 99% as well.
What society do we wish to leave for our children to take control over when they are grown up?
Perhaps this is the basic question we need to take more serious. Perhaps we find that only by taking to the streets we might have a chance to bring the changes that we wish to bring forward. Politicians will have to react to the pressure from the streets, whether it is by tears gas, or by political change, reactions will follow. It is a numbers game really, the threshold passed which ignorance does no longer work, and reactions must follow.
The ritual of the G20 stage managed final summit photo. Smiling people facing death, starvation, poverty and injustice, the extended arms of Bankers interests.
They do not represent me, not a sausage! They represent what is wrong with our system, like the IMF and World Bank represent what is wrong. Conscience to me Malcolm, is not exclusively a matter of intellect, think Sophocles's Antigone.
Disobedience is a matter of conscience, and equally a conflict of course. I believe that the post WWII consumerism that dominated our societal structures has hindered the healthy development of critical conscience in generations, this is only one explanation for the wide spread political ignorance and the will to subscribe to propaganda exclusively.
In my world, conscience is the glue that hold together civilization, the more we loose it, the more we endanger civilization. In the age of enlightenment, Kant expressed critical conscience in the categorical imperative.
I believe we are at the crossroad where one way is into another age of enlightenment or the other points back to the dark ages. As the human beings that we are, the choice is ours.
Perhaps, it's time for Greece to call in Rufus T. Firefly, or has it been him in charge all along?
The German haircut plan has effectively made Greece bankrupt(you can't suggest a haircut without saying bankruptcy in the same breath). Problem is that the so called Greek haircut is only 1/40th of total eurozone problem that Germany needs to cure. Therefore Germany has both failed to cure the eurozone problem (grossly inadequate measures) and has thrown Greece into bankruptcy. This is the most malicious act I have ever witnessed during my lifetime.
One question , what's Fitch and S&P says if the Oct 27th agreement is implemented ? It is DEFAULT isn't it ?
As soon as PSI exchange is carried out , Greece is going to be declared by rating agencies as Default .
It's not only Germany Dean , US on the other hand is using Greece as a blunt instrument to extort Germans .
What really makes me angry is the plan of german elite for Greece . It is in every aspect COLONIAL . HELIOS is a disgrace ! What we need to do , in my opinion , is to inform other european people about the "Bail out" and the "investment plan" prepared for Greece .
I show them documents and they feel ashamed by what their government is doing . That's the only way , i am afraid . Fight the propaganda in international media .
The same as Varoufakis is doing for several months now !
The next one is to contrast the previous one .
When all else fails there is art. Going out on a giant limb here (as the topic of this blog is economics/politics last I checked) I post one of my poems, below. Written a few years ago and inspired by another occasion, it seems perfect (unfortunately) for this week's occasion as well.
When they are moving their lips?
To serve the ball again.
The haircut plan to me seems the only option. The debt mountain is just far too big. For a while now, EU partners tried the way of giving emergency loans. Doesn't work as, with the economy shrinking while trying (unsuccessfully so far) to balance the budget – which is one precondition to stop the debt mountain from growing – the debt/GDP ratio keeps increasing.
So the debt mountain has been growing and continues to do so, despite Greek effort to balance the budget and EU emergency loans.
Reason is that a substantial part of the Greek pre-crisis GDP was based on debt-fuelled growth. With balancing the budget, that part of GDP (20ish percent?) just disappears. Together with the debt mountain that already existed before the crisis and the fact that even now, the budget is not balanced, the debt situation is truly unsustainable.
So "Plan A" did not work. Therefore, we need a Plan B. The only way out I can see is to reduce debt. As Greece isn't able to grow out of it (economy was already debt-supercharged and that "turbo" is gone now) and can't pay it off by increasing government revenue and/or quickly enough cutting the budget, Greece is truly insolvent.
A haircut is the only option out of this mess.
Apart from Germany (and others – volunteers first!) just handing over the money. But we don't have money just pouring out of the ground (like Saudi Arabia). So just giving the money away to a country that's been cheating all along and seems deeply dysfunctional would just throw good money after bad wouldn't be right.
A haircut is a bad thing. But the best solution for everybody in this situation.
@Martin Can you give me some numbers with the projection of greek financial situation with haircut of 27th October applied ? Does this agreement turn the greek debt sustainable ?
Also , i would really like your opinion about the insolvency issue of German and French banks . Are you aware of this matter ? Has your prime minister informed you about your financial status ?
On the other hand, throughout his blog he has been explaining why the haircut is not going to solve anything. And his prediction proved to be correct, since right after the Oct 27 Agreement Italy's fall accelerated instead of stopping (even before the Greek referendum fiasco).
No, I unfortunately don't have a projection of the Greek situation with the haircut applied. I've read somewhere that the debt / GDP ratio may go down to 120% (currently at about 160%).
Anyway, without the agreement, the debt mountain (now at around 160% of GDP) is bound to keep growing.
Unless something dramatic happens to lower the debt (by e.g. Greece applying a one-time "emergency wealth tax" to its wealthier citizens, using the Gold reserves to pay down debt or whatever). But this does not seem to happen. So without a haircut, Greece would just need more and more "emergency loans" and the debt mountain would keep increasing.
Taking 50% of the debt off (applied to some of the debt but not all of it) as foreseen in the October agreement would obviously lower the debt.
So – together with other drastic measures that Greece has to take (see above for some suggestions) – there is a higher chance that the debt could be stopped from growing. And sometime, from a lower base, the economy would start growing again and the debt / GDP ratio would start going down (slowly).
But given the experience of the endless negotiations and the Greek lack of leadership as well as some common understanding within the population that drastic measures have to be taken and are inevitable to get out of this situation (as well as some social balance by having the wealthier ones carry a bigger burden than the less fortunate ones), I don't think the October agreement would finally lead to the desired result.
So that's why I suggest: Let's accept that this is not working. Stop pumping "loans" into Greece that will never be paid back. Just let Greece default, have a massive haircut (more than 50% on all debt), switch to the Drachma and then try again.
This does not work so we should stop trying. It is painful and degrading not only for Greece but also for the rest of Europe.
Europe's limited resources should be applied where hopefully, they can still make a difference: Maybe Italy can still be saved. But Greece is beyond any cure within the Eurozone, I believe.
This would cost some money in order to support some otherwise failing e.g. French and German banks. But so be it. That would be a one-time expense while keeping to pay for Greece would go on for years and years to come. And in the end, it won't even work and the Greek hate us anyway. So why not stop what does not work?
I agree. We need to fight back. This is a communications war; we didn't choose this fight but we are deeply in it and we are losing horribly at the moment.
See my comment on one blog above(more recent).The PSI needs to be removed from the Greek package. It's the PSI that causes the default. Germany can do better than this and let's stop pretending that there is only one way to resolve the crisis (and that is Germany's way and that's it).


Is it possible to graphically view free space in FS viewer?
Save as .doc damn you!!!
Evolution - Change Data Locations?
Stable Alternative to Internet Explorer?
Is there any VM software that uses Intel's VT yet?
Mplayer "Error opening/initializing the selected video_out(-vo) device"


text:
\section{Introduction}\label{sec:introduction}

In the recent years, a large number of surveys have obtained multi-wavelength
imaging and spectroscopy for large samples of galaxies at different redshifts. Thanks to these surveys,
we have learned a lot about how galaxies form and evolve.
However, many physical  processes, such as the regulation of star formation by gas accretion,
remain poorly understood.

The accretion of cold gas in the form of gas-rich
dwarf galaxies can  bring gas to galaxies and fuel star formation
\citep[]{Sancisi-08,Silk-Mamon-12,Conselice-13}.
The presence of extra-planar gas \citep[]{Chaves-Irwin-01, Boomsma-05, Wakker-07},
lopsided H{\sc{I}} morphologies \citep[]{Sancisi-76, Shang-98, Thilker-07}
and gas tails \citep[]{Kregel-Sancisi-01, Oosterloo-10} may directly be
linked to ongoing cold gas accretion through mergers.
While some portion of the gas in galaxies is being acquired through the
accretion of dwarf galaxies, the inferred gas accretion rate is not sufficient
to sustain star formation in galaxies ($\sim1.0\,{\rm M_{\odot}}\,{\rm yr}^{-1}$)
\citep{Binney-Dehnen-Bertelli-00}. As a consequence, a large  fraction
of gas should be accreted directly from the Intergalactic Medium (IGM).
Low-density galaxies  lose their gas through tidal interactions or ram pressure
stripping, which may finally quench their star formation
\citep[]{Moore-96, Calcaneo-Roldan-00, Mayer-06, McCarthy-08, Kapferer-08, Chang-Maccio-Kang-13}.
This process happens more frequently in dense environments.

The Bluedisk project, which was carried out  with the Westerbork Synthesis Radio Telescope(WSRT), was  designed to
map the H{\sc{I}} distribution is a sample of 25 unusually H{\sc I}-rich  galaxies.
Galaxies with large  H{\sc{I}} excess
usually have bluer and younger outer disks \citep{Wang-11}, and more metal-poor ionized gas \citep{Moran-12}.
A sample of 25 control galaxies was  also observed for
comparison. These galaxies were closely matched in stellar mass, stellar surface mass density,
redshift and inclination, but were not unusually rich in H{\sc I}. The goal of the project was to
determine whether there was any evidence for recent gas accretion onto unusually H{\sc I}-rich galaxies by
investigating and contrasting the  H{\sc{I}} structure and environment of the gas-rich galaxies
with that of the control sample.

In the first paper of Bluedisk project, \citet[Paper I]{Wang-13} concentrated
on the H{\sc{I}} size and morphology of the 42 targeted galaxies. They found
that H{\sc{I}}-rich galaxies do not differ from normal
galaxies with respect to H{\sc{I}} asymmetry indices or optical/H{\sc{I}}
disk position angle differences. This is inconsistent with a scenario in which
the excess gas was  brought in by mergers. In this paper, we extend
this work to the galaxies in the neighbourhood of the targeted galaxies that lie within
the WSRT data cubes.

Our paper is organized as follows. In section 2, we briefly recap our observations, describe the
data and the data processing that we carried out for our  environmental study, including
our procedure for  accurate
primary beam correction.
In section 3, we discuss our identification of galaxy neighbours  via cross-matching with the
spectroscopic catalogue of the Sloan Digital Sky Survey (SDSS) and how we
build a uniform catalog of these sources.
In section 4, we examine the H{\sc{I}} mass-size relation and the correlation between
H{\sc I} and optical properties such as mass and stellar surface density for both the
neighbours around H{\sc I}-rich and control galaxies.
In section 5, we discuss the morphology and properties of galaxies which are found to be outliers from
the standard scaling relations.
We summarize our results in section 6.

Throughout this paper, all the distance-dependent
parameters are computed with $\Omega=0.3$,
$\Lambda=0.7$ and $H_0= 70$ km s$^{-1}$ Mpc$^{-1}$.

\section{Data}

\subsection{Observation and data reduction}
The 50 targets were observed with the WSRT in 2011 and 2012. Target selection and
data reduction are described in detail in Paper I. For  detailed information
on the targeted galaxies we refer the reader to table 1 in Paper I.

The H{\sc{I}} raw data cubes were reduced using a
pipeline produced by \cite{Serra-12}, based on the Miriad
reduction package \citep{Sault-Teuben-Wright-95}.
The data used in this paper are H{\sc{I}} cubes built with
a Robust weighting of 0.4, which provides a suitable compromise between
sensitivity and resolution. The pixel size is
4 arcsec and the velocity width for each channel is about
$13$ km s$^{-1}$. The velocity resolution is $26$ km s$^{-1}$ (FWHM).
The typical beam has Half-Power Beamwidth (HPBW) of $16\times16/$sin($\delta$) arcsec$^2$,
where $\delta$ is the declination.
Every cube has 148 channels,  covers a redshift
range of $\Delta z=0.006$, and  has a size of 1 degree on each side, which
corresponds to a physical scale of 1.7 Mpc at a redshift $z=0.025$.
We point out that 92.0\% of the galaxies are within a systematic velocity
difference of 500 km s$^{-1}$ from the primary galaxies. However, some
untargeted galaxies are not in the immediate neighborhood of the primary
 galaxies: in the radial direction, the farthest galaxy is 884 km s$^{-1}$ away.
 Hence we are investigating a relatively large-scale environmental effect
 rather than the direct interaction between galaxy pairs in this paper.

We generate two-dimensional H{\sc{I}} total-intensity maps
(moment-0 maps) for each cube. First we identify 3-d regions of emission by a smoothing and clipping
algorithm. We then add all the
detected H{\sc{I}} emission from  all velocity channels.
We also estimate errors for all non-zero pixels in the H{\sc{I}} intensity map.

\subsection{Physical properties of galaxies}
The  physical quantities required for this work are a spectrophotometric estimate of the stellar
mass $M_{*}$, stellar surface mass density $\mu_{*}$, and the NUV-r colour.
Stellar masses were taken from the MPA-JHU database (http://www.mpa-garching.mpg.de/SDSS/DR7/),
and are derived from Sloan Digital Sky Survey (SDSS) photometry. The stellar surface mass density is defined as
$\mu_{*}=M_{*}\,(2\pi R_{\rm 50,z}^2)^{-1} $, where
$R_{\rm 50,z}$ is the physical radius which contains half the
total light in the z-band. The NUV magnitude is available from the Galaxy Evolution Explorer (GALEX)
pipeline and the NUV-r colors are corrected for Galactic extinction.
The H{\sc{I}} size $R1$, $R_{\rm 50,H{I}}$,
$R_{\rm 90,H{I}}$ and $rs$, and H{\sc{I}} mass $M_{\rm H{I}}$,
are measured using  our H{\sc{I}} data cubes. $R1$ is
the radius where radially averaged face-on H{\sc{I}} column density
reaches $1\,{\rm M_{\odot}}\,{\rm pc}^{-2}$(corresponding to $1.25\times10^{20}$atoms cm$^{-2}$).
$R_{\rm 50,H{\sc I}}$ and $R_{\rm 90,H{\sc I}}$ are the radii enclosing 50 and 90 percent of the H{\sc{I}} flux,
respectively. Note that an inclination correction is not applied when calculating $R1$
for unresolved galaxies ($R_{\rm 50,H{\sc I}}$ less than 15 arcsec), because their H{\sc{I}} sizes
are less than the beam size. For these galaxies, the derived value of $R1$
should be regarded as an upper limit to the true value of $R1$.
$rs$ is the scale-length of the  outer exponential disk,
and is measured by assuming a PSF-convolved two-component model for  the radial distribution
of H{\sc{I}} (see Wang et al. 2014 for details).
The H{\sc{I}} mass is defined as
$M_{\rm H{\sc I}}$=$2.356\times10^5$($D_{\rm lum}\,{\rm Mpc}^{-1}$)$^2$($F_{\rm tot}\,{(\rm Jy\,km\,s^{-1}})^{-1}$),
where $D_{\rm lum}$
is the luminosity distance
and $F_{\rm tot}$ is the integrated H{\sc{I}}-line flux density.
The measurements of these parameters are described in more  detail
in Paper I.

\subsection{Primary beam correction}

\begin{figure*}
\centerline{
    \includegraphics[width=0.45\textwidth]{plots/com.pdf}
    \includegraphics[width=0.45\textwidth]{plots/com3.pdf}}
\caption{Test of the two methods for  primary beam correction:
1) applying the standard WSRT analytic model (with $c$=63),
and 2) a nonparametric model by Popping \& Braun (2008).
This figure shows the relation between the primary beam
corrected flux density and the FIRST/NVSS flux density.
Black circles and blue crosses represent the FIRST data and the NVSS data,
respectively. The left and right
panels are for Popping's model and the empirical model, respectively.}
\label{fig1}
\end{figure*}

Our work depends critically on the primary beam correction, which accounts for the
attenuation by the primary beam towards large radii. We consider two methods.
One is a non-parametric model (data cube)  provided by \cite{Popping-Braun-08},
the other one is to apply a parametric correction function of the form $\cos^6(c\times \nu\times d)$
as routinely used for the WSRT, where $\nu$ is the frequency in GHz,
and $d$ is the angular distance from the pointing centers in degrees.

To test and calibrate both approaches, we compare the un-corrected flux densities of point
sources in the radio continuum maps, which are an additional product of our data reduction
pipeline (see Wang et al. 2013) with the flux densities listed in the NRAO FIRST
 \citep[Faint Images of the Radio Sky at Twenty-Centimeters]{Becker-White-Helfand-95}
and NVSS \citep[NRAO VLA Sky Survey]{Condon-98} catalogues.

Specifically, we first extract sources from
our continuum maps using Source Extractor (SE). Then we use the point spread function (PSF) fitting
method to derive the flux density of each source extracted from our continuum
maps. With a detection threshold of $5\sigma$, where $\sigma$ is the rms noise with a typical value
of $8.0\times 10^{-5}$ Jy beam$^{-1}$, we extract more than two thousand sources from all images.
This catalog is then matched to the FIRST
and NVSS catalogs. In total, there are 4128 sources in the FIRST
catalog \citep[12Feb16 Version]{Becker-12} located in these 50 H{\sc{I}}
observed regions, with integral flux density greater than 1 mJy.
Among them, 1322 sources are classified as point sources
at FIRST resolution (with a major axis FWHM of 2 arcsec).
About one hundred detections in our cubes were matched with both FIRST
and NVSS point sources. We restrict the analysis to point sources because
FIRST and NVSS flux densities are very
consistent with each other for point sources, with a scatter of 0.05 dex.

This way, we obtain an best-fit $c$ of 63, differing distinctly from the commonly used
and recommended $c=68$ (see WSRT web pages). This difference in $c$ causes a
0.46 dex difference in flux intensity for pixels at the farthest edge of the
continuum map (0.71 degree from the map center at redshift $z=0.025$),
and a largest difference of 0.17 dex for our farthest detected source.
On average, the flux densities corrected with $c=63$ are 0.04 dex smaller
than that of $c=68$ for our untargeted sources.
Fig. 1 shows the comparison between the primary beam corrected
PSF flux densities from our continuum maps and
the FIRST/NVSS flux densities using both methods, the empirical analytic (standard) model,
and Popping's nonparametric model.
We can see a good linear correlation
between the corrected PSF flux density and the FIRST/NVSS data. It is difficult to tell which
model is better according to the data points, because the scatter is
similar ($\sim$ 0.7 dex).  However, we remark that the standard
recommended analytic model with $c=68$ would have provided an insufficient primary
 beam correction in the wavelength range considered in this work.
Since we confirm that the model of \citet{Popping-Braun-08} works well, we adopt it for our primary beam
correction for the Bluedisk data cubes.

\section{Source identification}

We use the source finder developed by \citet{Serra-12} to detect sources
 in the cubes. The pipeline uses a smooth-and-clip algorithm: it smooths
the cube and searches for regions with a flux intensity above 3$\sigma$ of
 the cube. The resulted catalog of 1962 sources includes both real sources
 and noise peaks. We take a few steps to filter the real galaxies with
reliable flux measurements. The first step is to match the H{\sc I} catalog with
the SDSS spectroscopic catalog. 163 H{\sc I} sources are matched with optical
galaxies, with an angular distance smaller than 20 arcsec (roughly the
beam size). 10 of them have more than one matched optical counterpart.
We further constrain in redshift by requiring $|z_{\rm spec}-z_{\rm H{\sc I}}|<0.001$,
which left us with 120 H{\sc I} sources, and none of them have multiple
optical counterparts.  Although we may miss the galaxies with no optical
 spectroscopic observation, we efficiently exclude most of the unreliable
 sources from the H{\sc I} catalog.

In the following sections, we describe how we further select the sources
 with reliable H{\sc I} flux measurements.

\subsection{Defining the outermost H{\sc{I}} contour}

\begin{figure*}
\centerline{
    \includegraphics[width=0.32\textwidth]{plots/snr.pdf}
    \includegraphics[width=0.32\textwidth]{plots/limit.pdf}
    \includegraphics[width=0.32\textwidth]{plots/limit_num.pdf}}
  \caption{  The left panel shows the SNR varies with applying different column density limits.
The middle panel shows the flux fraction varies with increasing column density limit. The flux fraction is the ratio of
the total H{\sc{I}} flux above a specific column density limit to the H{\sc{I}} flux without
giving a column density limit.  The right panel shows the
column density limit versus the fraction of retained sources. The color
curves represent different pixel number cuts (If the effective pixel
number of the source is greater than the cut, it is treated as
a source).\label{fig2}}
\end{figure*}

In Paper I, we describe how we build error maps for the H{\sc{I}} moment-0 images.
We use these error maps to determine a H{\sc I} column density threshold
that reliably defines an outermost contour for  morphological analysis.
The outermost contour should also  contain most of the total flux of the
source.
The left panel of Fig. 2 shows the signal-to-noise ratio at different H{\sc I} column density levels
for all the detected sources.
The black curve shows the median signal-to-noise ratio,
 and the gray region shows the 20\% to 80\% percentile range.
The SNR is typically above 3 when the threshold is set to be $10^{20}$ atoms cm$^{-2}$.

The middle panel of Fig. 2 shows how the fraction of the total flux of the galaxy
varies as a function of column density limit.
The back curve shows the median flux fraction for all sources, and
the gray region shows the 20\% to 80\% percentile range.
\footnote {At a column density limit of zero,
the H{\sc{I}} flux fraction is larger than 1.0 for all galaxies,
 because by clipping at that level, the noise contribution is neglected (i.e., some negative
total flux from negative noise peaks has to be added to counterweight this effect at the edges of
the detected sources.}
We see that most of the galaxies retain more than 90\% of their
total flux when the limiting contour
level is $10^{20}$ atoms cm$^{-2}$.

We require sources to contain at least 20 pixels in the moment-0
maps to be included in our catalogues. In the right panel of Fig. 2, we show the fraction
of sources that meet this criterion as a function of different density
threshold cuts (the black curve). We also show how the curve changes if we
change the resolving criteria to 10, 30 and 40 pixels.
We can see more than 90\% of the sources are resolved with 20 pixels at
a density detection threshold of $10^{20}$ atoms cm$^{-2}$.

Based on the analysis shown above, we adopt  $10^{20}$ atoms cm$^{-2}$
as our H{\sc I} column density threshold, because it is demonstrated to be  a good threshold for
reliably describing the shape and size  of the H{\sc{I}} while  still retaining most of
the H{\sc{I}} mass, and it also includes most of the well-resolved H{\sc{I}} sources.

\subsection{Extracting sources with reliable H{\sc{I}} fluxes}

\begin{figure*}
  \includegraphics[width=0.45\textwidth]{plots/scatter.pdf}
  \includegraphics[width=0.45\textwidth]{plots/scatter1.pdf}
  \caption{ The left panel shows the changing of H{\sc{I}} flux scatter with different H{\sc{I}} flux bins for
simulated sources.
The right panel shows the distributions of H{\sc{I}} flux ratio for different H{\sc{I}} flux
intervals for simulated sources. The black histogram represents the distribution of H{\sc{I}} flux ratio
 for H{\sc{I}} flux greater than 0.5 Jy km s$^{-1}$, and the red dot-and-dash histogram is for galaxies
with H{\sc{I}} flux less than 0.5 Jy km s$^{-1}$. Besides, the red
histogram is also for galaxies with H{\sc{I}} flux less than 0.5 Jy km s$^{-1}$, but with SNR greater than
3. \label{fig3}}
\end{figure*}

To estimate the reliability of our determinations of the total H{\sc{I}} flux, we use a bootstrap method. We
simulate a set of repeat observations by adding random noise with
the same characteristics as the noise in the Bluedisk cubes, and measure the
resulting variance if the  total H{\sc I} flux.
In practice, we take the channels that have no detected sources from the data cube, and randomly repeat
them to make noise cubes that have the same size as the Bluedisk data cubes. We add the noise cubes to the original
Bluedisk cubes to make a ``perturbed'' cube. We repeat this process 10 times for each original Bluedisk
cube.
In addition, we also generate error maps for these simulated cubes.

The left panel of Fig. 3 shows how the scatter in the derived H{\sc{I}} between the different perturbed cubes varies
function of the original fluxes. The H{\sc{I}} flux scatter rises sharply for H{\sc{I}} fluxes
less than 0.5 Jy km s$^{-1}$, and becomes almost flat at a value of about 0.04 dex for H{\sc{I}} fluxes greater than
0.5 Jy km s$^{-1}$.

The right panel of Fig. 3 shows the distribution of the ratios of simulated H{\sc{I}} fluxes and input H{\sc{I}} fluxes
in two flux bins. The black histogram shows the ratio of the distribution for galaxies with H{\sc{I}} fluxes greater
than 0.5 Jy km s$^{-1}$, and the red dot-and-dash histogram shows the distribution for galaxies with H{\sc{I}} fluxes less
than 0.5 Jy km s$^{-1}$. The simulated H{\sc{I}} fluxes in the lower H{\sc{I}} flux bin are clearly more scattered than
in the higher H{\sc{I}} flux bin. We further select galaxies that have a SNR of at least 3 for the
$10^{20}$ atoms cm$^{-2}$ H{\sc I} column density contour. The distribution of their flux ratios
is shown as the red histogram in Fig. 3.
We find it to be similar to that of galaxies with high H{\sc{I}} flux.
In what follows,  we exclude low H{\sc{I}} flux sources (total H{\sc{I}} fluxes less than 0.5 Jy km s$^{-1}$) with
a SNR of less than 3 in the $10^{20}$ atoms cm$^{-2}$ contour.
Our tests show that  this ensures that
the error in the   H{\sc{I}} fluxes we measured will be less than about 0.04 dex.

There are 43 targeted galaxies and 65 additional galaxies
in the final sample. Among the galaxies that were not targeted, 45 galaxies are resolved
and 20 galaxies are unresolved. Among these additional galaxies, 15 galaxies are located in
the ``peculiar cubes'' \citep{Wang-13}, in which the targeted galaxy is not detected
in H{\sc{I}} or is otherwise disturbed. We exclude these galaxies
in the analysis described below. We also divide our targeted galaxies into two parts according to
whether they lie above or below the H{\sc I}-plane defined in \cite{Catinella-10}.
Hereafter, targeted galaxies
which lie above the H{\sc I}-plane are referred to H{\sc I}-rich galaxies (blue sample)
and the cubes they reside in are referred as blue cubes.
Similarly, the rest of targeted galaxies are referred as control sample and the rest of cubes are
referred as control cubes.
This definition is different to what was designed in observation, but it properly reflects
the actual H{\sc I} content of each system.
At last, 23 blue targeted galaxies, 20 control targeted galaxies, 26 untargeted galaxies in blue
cubes and 24 untargeted galaxies in control cubes are left.

The detailed properties of all the additional detected galaxies are listed in table 1.
Galaxies in ``peculiar cubes'' are also listed in this table, but not used for
 analysis in the following part of the paper.
As can be seen, they span stellar masses from $10^8-10^{11} {\rm M_{\odot}}$ and H{\sc I} masses from
$10^{8.5}-10^{10.4} {\rm M_{\odot}}$.
Although our sample is small in size, it is unique in that it samples the environments
rare, very H{\sc I}-rich systems.
Most of the  galaxies are resolved in H{\sc{I}}, enabling us to
study their resolved morphology and their kinematics. Compared to the Westerbork observations of neutral Hydrogen
in Irregular and SPiral galaxies (WHISP), our data are more sensitive.
\\
\begin{table*}
\begin{center}
\renewcommand{\arraystretch}{0.9}
\begin{tabular*}{1.0\textwidth}{c c c c c c c c c c c c c}
\hline \hline
 \multicolumn{1}{c}{ID} &\multicolumn{1}{c}{ra} & \multicolumn{1}{c}{dec} & \multicolumn{1}{c}{z} & \multicolumn{1}{c}{$\log M_*$} & \multicolumn{1}{c}{$\mu_*$} & \multicolumn{1}{c}{NUV-r}  & \multicolumn{1}{c}{$\log\,M_{\rm H{\sc{I}}}$} & \multicolumn{1}{c}{$Dis$}& \multicolumn{1}{c}{$R1$} & \multicolumn{1}{c}{$R_{\rm 50,H{\sc I}}$} & \multicolumn{1}{c}{$R_{\rm 90,H{\sc I}}$} & \multicolumn{1}{c}{$rs$} \\
\multicolumn{1}{c}{ } &\multicolumn{1}{c}{ } & \multicolumn{1}{c}{ } & \multicolumn{1}{c}{ } & \multicolumn{1}{c}{$\rm M_{\odot}$} & \multicolumn{1}{c}{$\rm M_{\odot} kpc^{-2}$} & \multicolumn{1}{c}{ }  & \multicolumn{1}{c}{$\rm M_{\odot}$} & \multicolumn{1}{c}{degree}& \multicolumn{1}{c}{arcsec} & \multicolumn{1}{c}{arcsec} & \multicolumn{1}{c}{arcsec} & \multicolumn{1}{c}{arcsec} \\
\hline
  14 &  112.31934 &   42.27963 &  0.02307 & 10.39 &  8.33 &  2.87 &  9.88 & 0.30 &   61 &   31 &   57 &   3.8 \\
  78 &  123.48852 &   52.64847 &  0.01820 & 11.01 &  8.99 &  3.80 & 10.40 & 0.22 &  140 &   63 &  132 &  16.4 \\
  84 &  123.03966 &   52.45524 &  0.01874 &  9.61 &  8.14 &  2.03 &  9.55 & 0.16 &   46 &   23 &   41 &     - \\
 143 &  127.30350 &   40.85448 &  0.02510 &  9.33 &  7.74 &  2.49 &  8.77 & 0.21 &   16 &   12 &   21 &  37.0 \\
 179 &  127.73492 &   55.83517 &  0.02542 &  8.91 &  7.53 &  2.56 &  8.73 & 0.39 &   15 &   11 &   21 &   6.1 \\
 221 &  129.17748 &   41.47231 &  0.02919 &  9.88 &  8.29 &  1.94 &  9.80 & 0.08 &   42 &   24 &   46 &  11.9 \\
 248 &  129.80326 &   30.92383 &  0.02569 &  8.51 &  7.10 &  2.03 &  9.19 & 0.19 &   23 &   17 &   31 &  15.4 \\
 306 &  132.05204 &   36.78074 &  0.02527 & 10.24 &  8.49 &  2.52 &  9.46 & 0.24 &   32 &   16 &   29 &   4.1 \\
 307 &  132.66660 &   36.46876 &  0.02521 &  6.98 &  6.98 &  1.51 &  9.94 & 0.35 &   57 &   25 &   55 &     - \\
 346 &  132.02870 &   41.85922 &  0.02997 & 10.11 &  7.99 &  2.64 &  9.53 & 0.26 &   32 &   21 &   36 &     - \\
 370 &  137.21930 &   44.93228 &  0.02657 & 10.27 &  9.31 &  3.62 &  8.96 & 0.13 &   14 &   14 &   43 &   7.9 \\
 375 &  137.33753 &   45.03975 &  0.02730 &  8.89 &  7.25 &  1.63 &  9.55 & 0.26 &   37 &   17 &   31 &   7.3 \\
 394 &  138.20927 &   40.49874 &  0.02759 &  9.60 &  8.03 &  2.17 &  9.73 & 0.41 &   37 &   18 &   37 &   7.4 \\
 396 &  138.39333 &   40.46574 &  0.02758 &  8.59 &  7.12 &  1.93 &  9.34 & 0.35 &   27 &   16 &   26 &   4.8 \\
 444 &  138.37436 &   51.31519 &  0.02773 &  8.80 &  7.25 &     - &  9.33 & 0.23 &   25 &   13 &   27 &  28.8 \\
 446 &  138.53751 &   51.41797 &  0.02805 &  9.51 &  8.59 &     - &  9.17 & 0.14 &   21 &   14 &   32 &   8.7 \\
 454 &  138.84323 &   51.05039 &  0.02881 &  9.68 &  7.78 &  2.41 &  9.45 & 0.32 &   31 &   19 &   28 &   4.3 \\
 482 &  139.35935 &   45.97174 &  0.02574 &  9.45 &  7.89 &  2.80 &  8.49 & 0.20 &    6 &   14 &   28 &  22.2 \\
 483 &  139.55919 &   45.65171 &  0.02690 & 10.70 &  8.47 &  2.87 & 10.16 & 0.30 &   68 &   35 &   61 &   5.0 \\
 517 &  139.90499 &   32.35320 &  0.02652 &  9.72 &  8.54 &  2.01 &  9.25 & 0.23 &   24 &   18 &   45 &  11.3 \\
 563 &  141.20293 &   49.39827 &  0.02723 &  9.73 &  8.27 &  3.30 &  8.72 & 0.24 &   15 &   10 &   19 &     - \\
 773 &  153.03446 &   46.29371 &  0.02425 & 10.34 &  8.48 &  2.63 & 10.03 & 0.40 &   47 &   34 &   66 &     - \\
 776 &  152.84976 &   45.73539 &  0.02375 &  8.69 &  7.20 &  1.60 &  8.88 & 0.23 &   19 &   12 &   21 &     - \\
 840 &  153.80716 &   56.60331 &  0.02667 &  8.82 &  7.43 &  1.24 &  9.41 & 0.07 &   28 &   17 &   33 &   8.9 \\
 889 &  154.25328 &   55.88005 &  0.02437 &  9.77 &  8.28 &  2.34 &  9.56 & 0.28 &   36 &   18 &   33 &   6.7 \\
 941 &  153.81151 &   58.69174 &  0.02295 &  8.61 &  7.73 &  1.80 &  9.12 & 0.29 &    6 &   29 &   49 &   4.5 \\
 983 &  162.50634 &   36.25677 &  0.02190 &  9.75 &  8.09 &  3.12 &  8.47 & 0.09 &    6 &   17 &   27 &     - \\
 997 &  162.75426 &   36.19258 &  0.02380 &  9.85 &  7.80 &  2.23 &  9.98 & 0.23 &   55 &   23 &   47 &     - \\
 999 &  162.49449 &   36.41499 &  0.02327 &  9.50 &  8.20 &  3.34 &  8.78 & 0.08 &   17 &   13 &   24 &   5.7 \\
1020 &  166.86889 &   35.46365 &  0.02828 &     - &     - &  3.05 &  9.87 & 0.10 &   37 &   26 &   58 &     - \\
1022 &  166.95902 &   35.40299 &  0.02840 & 10.47 &  8.81 &  3.49 &  9.56 & 0.07 &   36 &   18 &   32 &  18.0 \\
1024 &  166.95821 &   35.68483 &  0.02846 & 10.30 &  9.10 &  2.97 &  9.62 & 0.22 &   41 &   25 &   42 &   9.1 \\
1027 &  167.10516 &   35.33068 &  0.02888 &  8.96 &  7.33 &  3.81 &  8.94 & 0.16 &   18 &   13 &   25 &     - \\
1042 &  168.52972 &   34.30886 &  0.02526 &  8.70 &  6.97 &  1.91 &  9.09 & 0.16 &   25 &   18 &   31 &  17.1 \\
1104 &  177.57556 &   35.25409 &  0.02128 & 10.22 &  8.97 &  2.84 & 10.08 & 0.36 &   68 &   35 &   76 &     - \\
1143 &  185.61022 &   40.76168 &  0.02292 &  8.40 &  7.68 & -0.14 &  9.14 & 0.17 &   28 &   16 &   27 &  16.9 \\
1183 &  193.23760 &   51.82684 &  0.02762 &  8.58 &  7.78 &  1.50 &  8.90 & 0.20 &   16 &   11 &   22 &  23.2 \\
1230 &  196.76312 &   57.86514 &  0.02874 &  8.77 &  7.04 &  2.04 &  9.09 & 0.27 &   19 &   12 &   22 &   4.6 \\
1254 &  198.42330 &   47.29923 &  0.02808 &  8.80 &  7.20 &  1.22 &  9.19 & 0.20 &   23 &   15 &   25 &   6.3 \\
1259 &  198.26018 &   47.34518 &  0.02841 &  8.76 &  7.28 &  1.79 &  9.02 & 0.11 &   17 &   14 &   30 &  10.4 \\
1261 &  197.86026 &   47.44052 &  0.02861 &  9.03 &  7.29 &  2.46 &  8.92 & 0.25 &   15 &    9 &   15 &     - \\
1296 &  198.84572 &   35.17351 &  0.02309 &  8.90 &  8.12 &  1.82 &  8.98 & 0.19 &   19 &   12 &   22 &   7.1 \\
1298 &  198.67004 &   35.03638 &  0.02374 &  8.67 &  7.46 &  1.61 &  9.21 & 0.28 &   22 &   14 &   29 &  13.2 \\
1323 &  203.28755 &   40.85307 &  0.02400 &  8.88 &  7.70 &  1.24 &  8.97 & 0.33 &   10 &   22 &   33 &   3.7 \\
1407 &  212.50986 &   38.70812 &  0.02576 &  9.86 &  8.31 &  3.81 &  9.67 & 0.21 &   34 &   28 &   52 &     - \\
1410 &  212.67758 &   38.71842 &  0.02561 &  8.57 &  7.42 &  1.30 &  9.26 & 0.18 &   23 &   19 &   47 &     - \\
1411 &  212.62710 &   38.73950 &  0.02606 &  8.95 &  7.86 &  1.23 &  9.44 & 0.15 &   29 &   16 &   31 &  12.5 \\
1414 &  212.69582 &   38.75970 &  0.02570 &  8.74 &  7.46 &  1.72 &  8.81 & 0.14 &   15 &   11 &   25 &     - \\
1415 &  212.72923 &   38.78592 &  0.02580 &  8.43 &  7.14 &  1.54 &  9.13 & 0.13 &   14 &   15 &   31 &   7.2 \\
1533 &  241.43411 &   36.27508 &  0.03123 &  9.40 &  7.50 &  1.74 &  9.79 & 0.30 &   44 &   23 &   38 &     - \\
1554 &  242.24289 &   36.61088 &  0.03014 & 11.02 &  8.83 &  3.33 & 10.42 & 0.31 &   26 &   50 &  104 &  26.6 \\
1605 &  246.16476 &   41.01995 &  0.02712 &  8.79 &  7.33 &  0.66 &  9.70 & 0.10 &   33 &   15 &   31 &   6.1 \\
1632 &  246.06271 &   41.11062 &  0.02926 &  9.97 &  8.21 &  3.27 &  9.70 & 0.22 &   38 &   17 &   33 &   9.6 \\
1639 &  246.70860 &   40.91786 &  0.02915 &  8.93 &  7.68 &  1.83 &  9.21 & 0.34 &   21 &   29 &   33 &   9.0 \\
1643 &  246.13086 &   40.68445 &  0.02943 &  8.80 &  7.49 &  1.10 &  9.06 & 0.28 &   20 &   18 &   36 &     - \\
1647 &  246.08427 &   40.86501 &  0.03000 &  9.34 &  7.50 &  2.46 &  9.13 & 0.16 &   17 &   12 &   44 &     - \\
1648 &  245.99846 &   41.13817 &  0.03029 &  9.08 &  7.39 &  1.34 &  9.59 & 0.27 &   34 &   17 &   33 &  20.6 \\
1663 &  250.62296 &   42.26285 &  0.02750 &  8.78 &  7.27 &  1.27 &  9.08 & 0.14 &   20 &   16 &   32 &  15.6 \\
1669 &  250.56263 &   42.05996 &  0.02780 &  8.82 &  7.68 &  1.96 &  9.17 & 0.22 &   20 &   18 &   50 &  19.7 \\
1700 &  251.48897 &   39.98583 &  0.03020 & 10.17 &  8.22 &  3.18 &  9.69 & 0.36 &    5 &   20 &   35 &   7.2 \\
1713 &  251.87396 &   40.56570 &  0.03108 &  8.92 &  7.44 &  1.39 &  9.68 & 0.32 &   37 &   19 &   32 &     - \\
1725 &  258.80617 &   30.45146 &  0.02864 &  9.98 &  8.17 &  2.56 &  9.66 & 0.31 &   39 &   20 &   34 &     - \\
1774 &  259.68221 &   58.13513 &  0.02908 & 10.95 &  8.85 &  3.60 &  9.98 & 0.39 &   55 &   26 &   48 &  13.5 \\
1795 &  258.77994 &   58.24045 &  0.03101 & 10.20 &  8.35 &  3.08 &  9.78 & 0.26 &   40 &   18 &   38 &     - \\
1907 &  262.17343 &   57.11476 &  0.02812 &     - &     - & -0.42 &  9.03 & 0.03 &   17 &   11 &   23 &  16.7 \\
\hline \hline
\end{tabular*}
\caption{Properties of additional galaxies extracted in
the data cubes of the  Bluedisk project. The detailed information
of the targeted galaxies is presented in Paper I.
 From left to right, columns represent galaxy ID, Right Ascension,
Declination, redshift, base-10 logarithm of the
 stellar mass, base-10 logarithm of the stellar surface density,
NUV--r color, base-10 logarithm of the H{\sc{I}} mass, distance to the
central of the data cube (in degree), $R1$, $R_{\rm 50,H{\sc{I}}}$,
$R_{\rm 90,H{\sc{I}}}$ and exponentially scale length rs,
respectively. }
\label{table}
\end{center}
\end{table*}

\section{Results}

\begin{figure}
  \includegraphics[width=0.45\textwidth]{plots/mass_dis1.pdf}
  \caption{ Stellar mass distribution of our sample.
The stellar mass is from the MPA-JHU DR7 catalogue. Our sample is
divided into BTG (blue), CTG (red),
BUG (green) and CUG (purple).\label{fig4}}
\end{figure}

The mass distribution for our final sample is shown in Fig. 4. The
sample is divided into four subsamples: the blue targeted galaxies (BTG)
, the control targeted galaxies (CTG), the additional
galaxies located in blue cubes (BUG) and the additional  galaxies located in control cubes (CUG).
By selection, all targeted galaxies are massive with $\log M_{*}/M_{\odot}>10$.
The additional galaxies have a very
broad stellar mass distribution from $10^8 \rm M_{\odot}$ to $10^{11} \rm M_{\odot}$.
The goal of this paper is to study their H{\sc{I}} properties.

\subsection{H{\sc{I}} mass-size relation}
\begin{figure*}
\centerline{
\includegraphics[width=0.45\textwidth]{plots/mass_scale1_cir.pdf}
\includegraphics[width=0.45\textwidth]{plots/mass_scale2_cir.pdf} }
\caption{ The H{\sc{I}} mass-size relation for our sample.
The left panel shows the mass-size relation for BTG (blue), CTG (red), BUG (green) and CUG (purple).
The right panel is similar to left one but for different stellar
mass ranges. Some outliers in H{\sc{I}} mass-size relation are
marked by their IDs (these galaxies are discussed in detail in section 5).}
\label{fig5}
\end{figure*}

The tight relation between the diameter of the H{\sc{I}} disk and the total
H{\sc{I}} mass in galaxies was investigated by \cite{Broeils-Rhee-97}. Later, it was found that
this relation changes very little for different kinds
of galaxies \citep{Swaters-02, Noordermeer-05}. Fig. 5
shows the H{\sc{I}} mass-size relation for our sample. The left panel shows
this relation for the four subsamples: BTG (blue),
CTG (red), BUG (green) and CUG (purple). The black line is from
\cite{Broeils-Rhee-97}. The right panel shows the same relation for different
stellar mass ranges. Some outliers far from this relation are
marked by their IDs.

Almost all the galaxies closely
obey this relation, which is consistent with the result of Paper I.
This relation is similarly tight for galaxies with both high and low stellar masses:
the average column density of H{\sc{I}} is about same for all spiral galaxies.
\cite{Wang-14} suggest that this relation is primarily a result of atomic-to-molecular
gas conversion in the inner disk and is further enhanced by a homogeneous radial distribution
of H{\sc{I}} density in the outer disk of galaxies. We will investigate the nature
of the handful of outliers later in the paper.

\subsection{H{\sc{I}}-optical scaling relations}

\begin{figure*}
\includegraphics[width=1.0\textwidth]{plots/fhi_mstar.pdf}
\caption{The H{\sc{I}} mass fraction plotted as a function of stellar mass,
stellar surface mass density and NUV-r for target
galaxies(black), other galaxies in the H{\sc I}-rich cubes (blue),
other galaxies in the  control cubes (red) and GASS sample galaxies (gray).
The black curve in the left panel shows the empirical relation of H{\sc{I}}
mass fraction as a function of stellar mass,
which is taken from \citet{Evoli-11}.}
\label{fig6}
\end{figure*}

\begin{figure*}
\centerline{
\includegraphics[width=0.45\textwidth]{plots/HI_plane_C10.pdf}
\includegraphics[width=0.45\textwidth]{plots/bias_dis_C10.pdf} }
  \caption{
Left panel: H{\sc{I}}-plane for our sample.
This panel illustrates that the ratio of H{\sc{I}} mass to stellar
mass versus the combination of surface mass density and NUV-r.
Galaxies in the BTG (blue), CTG (red), BUT (green), CUG (purple) samples are colour-coded.
The gray data points show  the GASS sample. Right panel: The distribution of
deviations from the  H{\sc{I}}-plane (corresponding to the black line
in the left panel) for our sample. The blue, red, green and purple distributions represent
for the distributions of BTG, CTG, BUG and CUG galaxies, respectively.
The K-S test probability for the difference in deviation from the H{\sc I}-plane
between the BUG and CUG samples is denoted at the top-right corner of the right panel.}
  \label{fig7}
\end{figure*}

\begin{figure*}
\includegraphics[width=1.0\textwidth]{plots/bias_center1.pdf}
\caption{The distributions of $\Delta$center, $R_{\rm 90,H{\sc{I}}}/R_{\rm 50,H{\sc{I}}}$, $rs$ and $rs/R1$ for BTG (blue),
CTG (red), BUG(green) and CUG(purple).
The K-S test probability that the H{\sc I}-rich and control cube
distributions are drawn from the same underlying distribution
is given in the top right corner of each panel.}
\label{fig8}
\end{figure*}

In Fig. 6, we plot the H{\sc{I}}-to-stellar mass ratio as a function of stellar mass,
stellar surface mass density and NUV-r color for our sample.
The H{\sc{I}} mass fraction correlates with stellar mass, surface mass density and NUV-r, and extends the
mean relations quantified for normal galaxies with stellar masses
greater than $10^{10} \rm M_{\odot}$ in former studies \citep[]{Catinella-10,Cortese-11,Huang-12}.
We do not see  different H{\sc{I}} scaling relations for  galaxies in the data cubes with
a central targeted  H{\sc{I}} excess galaxy and data cubes with a central targeted control galaxy.

We plot the H{\sc{I}} plane linking  H{\sc{I}}-to-stellar mass ratio with
stellar surface mass density and NUV-r colour defined by Catinella et al. (2010) in the
left panel of Fig. 7. The gray data points represent galaxies from
GASS \citep{Catinella-10}. In this projection,  both
targeted and untargeted galaxies lie close to the H{\sc{I}} plane.
Differences arise  when we focus on the {\em displacement} from the plane.
As already found in Paper I, we observe
a tilt of our observed galaxies with respect to the diagonal of the plot. The  plane underpredicts the
H{\sc{I}} content of all observed galaxies at the high-H{\sc{I}}-fraction end
and slightly over-predicts it at the low-H{\sc{I}}-fraction end of
our sample. The underprediction at the high-H{\sc{I}}-fraction end is discussed in detail by \cite{Li-12}, who argue
that the addition of additional parameters yield a more  unbiased prediction of H{\sc I} content.

The right panel of Fig. 7 shows the distributions
of the deviations from the H{\sc{I}}-plane (the black line in Fig. 7).
We find a significant difference between the distributions of the galaxies in the
cubes of the H{\sc I}-rich targets and the galaxies in the control cubes.
We perform a Kolmogorov-Smirnov (K-S) test to quantify this significance,
and obtain a probability of 0.041, suggesting a 96\% significance for the
 null hypothesis of the two samples being drawn from the same parent
distribution to be rejected.
It appears that on average, galaxies in the data cubes with an H{\sc{I}} excess
targeted galaxy do on average contain more H{\sc{I}} (relative to their
surface mass density and colour ) than galaxies
in the cubes containing a control galaxy.
 This suggests that galaxies associated with blue targeted galaxies are also likely to be gas-rich.
This supports the observation pointed out by \cite{Kauffmann-Li-Heckman-10},
see also \cite{Weinmann-06}, who found that there is
more photometrically estimated H{\sc{I}} in satellites around more star-forming primary galaxies than
in satellites around less star-forming primary galaxies. In the following, we refer to this as ``H{\sc{I}} conformity''.
 Those authors argued that the satellites trace a large-scale
gas reservoir that is accreted onto the central galaxies.

Next, we repeat the morphological analysis of Paper I for the additional galaxies detected in the cubes.
In Fig. 8, we plot  distributions of $\Delta$Center, $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$, $rs$ and $rs/R1$.
$\Delta$Center is calculated as the distance between the H{\sc{I}} center and the r-band center,
 normalized by the semi-major axis of the H{\sc{I}} ellipse.
$R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ describes the concentration/extension of the H{\sc{I}} disks.
$rs$ is the exponentially scale length of H{\sc{I}} disks.

The galaxies in the H{\sc I}-rich cubes do not differ from those in the control cubes in their distribution of
$\Delta$Center. However, their distributions of $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ do show a significant difference.
Galaxies in the H{\sc I}-rich cubes
 tend to have larger $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ than in the control cubes.
If we investigate galaxies with $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ greater than 2.0, we find almost all of them have more H{\sc{I}} gas than
the predicted by their optical properties. The distribution of the deviations from the H{\sc I}-plane for these galaxies
 is shown in Fig. 9. The median value of the deviations is 0.44 dex, which means these galaxies have 2.7
 times H{\sc I} of the predicted values in general.
 We also find their H{\sc{I}} to extend far beyond the optical disk.
The $rs$ and $rs/R1$ distributions of the galaxies in the H{\sc I}-rich cubes do not differ significantly from
those for galaxies in the control cubes.

To assess whether the density of the environment may play a role in these
differences, we checked the number of SDSS
spectroscopically observed galaxies of which fall in our cubes,
but which have no H{\sc{I}} detections.
There are 95 galaxies with no H{\sc{I}} detections in the H{\sc I}-rich cubes and 295 galaxies with no H{\sc{I}} detections
in the control cubes. Most of these galaxies have stellar masses in the
range between $10^8 \rm M_{\odot}$ and $10^{10} \rm M_{\odot}$.
We also quantify the environment by using the 3-d reconstructed matter overdensity
based on SDSS DR7 data set \citep{Jasche-10},
 which is defined as $\delta=(\rho-\bar{\rho})/\bar{\rho}$, where $\rho$ is the matter density and $\bar{\rho}$
is the mean matter density. Thus the mean overdensity of galaxies in control cubes is
10.7, while the mean over-density of galaxies in blue cubes is 4.6.
It is clear that the control cubes are located in denser regions than the H{\sc I}-rich
cubes, and the fraction of optically-identified galaxies that have detectable H{\sc{I}} masses is much higher in the blue
cubes than in the control cubes.
This may indicate that  H{\sc{I}} conformity is closely related to the environment of the galaxy.

\begin{figure}
\includegraphics[width=0.45\textwidth]{plots/plothist_con.pdf}
\caption{The distribution of deviations from the H{\sc I}-plane for untargeted galaxies with $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ greater than
2.0. The median value of these deviations is 0.44 dex.}
\label{fig9}
\end{figure}

\section{Morphology of outliers}

\begin{figure*}
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/0890_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/0890_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/0890_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/0941_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/0941_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/0941_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/0983_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/0983_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/0983_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1104_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1104_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1104_s.pdf}
}
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1323_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1323_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1323_s.pdf}
}\par
 \caption{H{\sc{I}} column density contours overlaid on optical images; H{\sc{I}} velocity maps and SDSS spectra for outliers.
 The galaxy ID, stellar mass and the predicted H{\sc{I}} mass fraction
 are labeled in the top-left-hand corner of each left panel.
 The white, green, red and yellow H{\sc{I}} contours represent 2.0, 4.0, 14.0 and 20.0 times
 the median SNR of the outermost contour, respectively.
 The shape of the beam is plotted in green at the bottom-right corner of each map. All the maps are displayed as
 north up and east left. }
 \label{fig10}
\end{figure*}

\addtocounter{figure}{-1}
\begin{figure*}
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1378_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1378_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1378_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1407_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1407_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1407_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1554_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1554_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1554_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1700_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1700_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1700_s.pdf}
}
 \caption{Continued}
\end{figure*}

\begin{figure*}
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/0220_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/0220_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/0220_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/0441_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/0441_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/0441_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1333_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1333_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1333_s.pdf}
}\par
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1662_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1662_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1662_s.pdf}
}
\mbox{
\includegraphics[width=0.25\textwidth]{plots/outliers/1663_m.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/1663_v.pdf}
\includegraphics[width=0.30\textwidth]{plots/outliers/SDSS/1663_s.pdf}
}\par
\caption{The same as Fig. 10 but for some of the non-outlier galaxies, selected
randomly from our sample galaxies with the offset to H{\sc I} mass-size relation less than 0.2 dex and the offset
 to H{\sc I}-plane less than 0.2 dex.}
 \label{fig11}
\end{figure*}

\begin{table*}
\begin{center}
\renewcommand{\arraystretch}{0.9}
\begin{tabular}{c c c c c c c c}
\hline \hline
\multicolumn{1}{c}{ID} & \multicolumn{1}{c}{Environment} & \multicolumn{1}{c}{$\log_{10} M_{\rm halo}$} & \multicolumn{1}{c}{H{\sc{I}} MS}  & \multicolumn{1}{c}{H{\sc{I}}-plane} & \multicolumn{1}{c}{$\Delta$Center} & \multicolumn{1}{c}{$R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$} \\
\multicolumn{1}{c}{ } & \multicolumn{1}{c}{ } &\multicolumn{1}{c}{$\rm M_{\odot}$}  & \multicolumn{1}{c}{dex} & \multicolumn{1}{c}{dex} & \multicolumn{1}{c}{ } & \multicolumn{1}{c}{}\\
\hline
941 & isolated & - &        1.15&     0.65  & 0.252 & 1.68 \\
1323 & -        & - &      0.51&   0.08  & 0.3981 & 1.51 \\
1554 & isolated & 12.59 &       0.97&     0.27  &0.350 & 2.09\\
1700 & isolated  & -     &       1.63&    0.15  &0.960 & 1.73\\
     &       &        &           &      &    &   \\
890 & isolated & 12.37 &      -0.14&    -0.87  & 0.447  & 1.85\\
983 & isolated & -     &       0.55&    -0.70  & 0.517 & 1.52\\
1104 & isolated & -    &     0.09&     0.66    & 0.129  &2.16\\
1378 & isolated & 12.37 &    -0.02&    -0.50   & 0.320 &1.76\\
1407 & -        & -     &     0.12&     0.62   & 0.517 & 1.87\\
\hline \hline
\end{tabular}
\caption{The list of outliers of H{\sc{I}} mass-size relation and H{\sc{I}}-plane.
 From left to right, columns represent galaxy ID, environment, halo mass,
 offset from normal H{\sc{I}} mass-size
 relation, offset from normal H{\sc{I}}-plane, $\Delta$Center and $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$, respectively.}
\label{table}
\end{center}
\end{table*}

\begin{figure*}
\includegraphics[width=0.9\textwidth]{plots/outlier_com.pdf}
\caption{The distributions of $\Delta$Center and $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ for outliers (red) and non-outliers (black).
The K-S test probability is given in the top right corner of each panel. The
non-outliers are selected from all the galaxies with both the offset to H{\sc I}
mass-size relation and the offset to H{\sc I}-plane less than 0.2 dex.}
\label{fig12}
\end{figure*}

Galaxies accrete cold gas directly from the intergalactic medium or through interaction with companions, and
lose their gas through tidal or ram pressure stripping.
Some authors have tried to connect specific H{\sc{I}} structures in galaxies with ongoing cold gas accretion, such
as the existence of extra-planar gas and warped structures of H{\sc{I}} distribution in
galaxies \citep[]{Wakker-07, Thilker-07, Oosterloo-10}.
Ram pressure striping, especially
in clusters also affect the morphology of H{\sc{I}} disks \citep[]{McConnachie-07,Bernard-12,Serra-13,Zhang-13}.
In this section, we investigate the structures of those galaxies which are outliers in the
H{\sc{I}} mass-size relation (see Fig. 5) or the H{\sc{I}}-plane (see Fig. 7).
We argue that (after close inspection) either offset is an indication for ongoing interaction
with the environment.

Outliers are defined to include galaxies that are offset in their H{\sc{I}} mass by more than 0.4 dex from the
normal H{\sc{I}} mass-size relation or offset more than 0.5 dex from the H{\sc{I}}-plane.
Here we just discuss the outliers with $M_{*}>M_{\rm H{\sc I}}$, since the H{\sc{I}} plane would underestimate
the H{\sc{I}} fraction for galaxies with $\log_{10}(M_{*}/M_{\rm H{\sc I}})>0$.
We select the outliers from all cubes with ``peculiar cubes'' (Section 3) excluded.
Note that there is no indication that outliers tend to fall preferentially into
either group of galaxies around H{\sc I}-rich galaxies (blue sample) or control galaxies.
In table 2, we list the environment of galaxies, host system Dark Matter (DM) mass, offset from the H{\sc{I}} mass-size
relation, offset from the H{\sc{I}}-plane, $\Delta$Center and $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$.
The environment of galaxies (isolated or in group) and
the host halo mass estimates are from \citet{Yang-07}.
Fig. 10 shows H{\sc{I}} total intensity contours overlaid on an SDSS colour image, an H{\sc{I}} velocity field and an SDSS
spectrum for each of these outliers. The white, green, red and yellow H{\sc{I}} contours
represent 2.0, 4.0, 14.0 and 20.0 times the median SNR of the outermost H{\sc I} contour, respectively.
The velocity fields are derived from a Gauss-Hermite fitting procedure (den Heijer et al., in preparation).

\subsection{Outliers in the  H{\sc{I}} mass-size relation}
 Galaxies marked 941, 1323, 1554 and 1700 are outliers from the H{\sc{I}} mass-size relation.
 Galaxy 1554 and 1700 are edge-on galaxies, while Galaxy 941, 1323 and 1622 are not.
 We will discuss Galaxy 941, 1323, 1554 and 1700 in detail.
 Galaxy 983 is investigated in next subsection because
 it is also offset from the H{\sc{I}} fundamental plane.

 \textbf{Galaxy 941 and 1323} are both starburst dwarf galaxies, but most of their H{\sc{I}} is distributed asymmetrically,
 and is also offset from the optical disks. The H{\sc{I}} of Galaxy 941 is distributed in patches
 that extend 10 times further than the optical disks. The nearby object seen in the SDSS image,
 is found to be a foreground star.
 The H{\sc{I}} disk of Galaxy 1323 shows a big void in the region of the optical disk.
 There are two possible explanations for these disturbed
 morphologies. One is feedback processes (by AGN or by superwinds powered by SNe and
 stellar winds in the starburst) that push gas from inside the galaxy to the outside.
 The other explanation is that the H{\sc{I}} gas in the stellar disk regions have been converted to  molecular gas
 to sustain the fast star formation, while the H{\sc{I}} gas in the outer regions has not had enough time to flow into the
 stellar disk.
 The stellar masses of the galaxies and their position on the ``Baldwin, Phillips \& Terlevich'' (BPT)
 diagram suggests that they do not  have AGNs  in their cores.
 We check the star formation time scale for these two galaxies.
 It would take more than 0.4 Gyr
 to consume ten percent of their total H{\sc{I}} gas with the current star formation rate.
 We conclude that SNe explosions and stellar winds are the most likely cause for
 the holes in the H{\sc{I}} intensity maps.
 In similar case, \cite{Muhle-05} argued that a huge hole in
 H{\sc{I}} distribution of NGC 1569 is probably driven from SNe feedback in the center of the galaxy over the past 20Myr.

 \textbf{Galaxy 1554 and 1700} are edge-on galaxies. As can be seen from the SDSS spectrum,
  the dust extinction is very high in Galaxy 1554.
  The H{\sc{I}} gas is concentrated and distributed in the stellar disk. Galaxy 1700 is a
  star-forming galaxy in which the  H{\sc{I}} seems to be vertically offset with respect to the stellar disk.
  The inclination correction creates significant  uncertainty when calculating H{\sc{I}} sizes
  for edge-on galaxies, since the H{\sc{I}} disks
  are usually thicker than stellar disks. This may result in the offset in the H{\sc{I}} mass-size relation.

\subsection{Outliers from the H{\sc{I}}-plane}

 \textbf{Galaxy 983} exhibits  a large offset from both the H{\sc{I}} mass-size relation and the H{\sc{I}}-plane.
 While it  appears to be H{\sc{I}} deficient with respect to the plane, its H{\sc{I}} is more concentrated
 than predicted by the H{\sc{I}} mass-size relation. In addition, a significant part of its H{\sc{I}} appears
 to show irregular kinematics and is offset from the galaxy disk. Hence, morphology and kinematics
 suggest recent tidal or ram-pressure stripping to have removed gas in the outskirts of the galaxy.

 \textbf{Galaxy 890} has its H{\sc{I}} gas compressed against the stellar disk on one side and
 extended to larger radius on the opposite side.
 Its morphological H{\sc{I}} and optical centers are distinctly offset from each other. This
 is very similar to the ram-pressure stripped
 galaxies observed in clusters \citep[]{Vollmer-04,Koopmann-Kenney-04,Crowl-05, Chung-09}.
 The observed  H{\sc{I}} gas mass is just 12\% of the predicted value.
 The velocity map shows a nice spider diagram in the optical region, marked in black ellipse (see Fig. 10).
 For the west extended part, which also contains most of the H{\sc{I}}, it shows a clear decrease in
 velocity from the inner region to the outer region.
 So it is likely that the direction of ram-pressure stripping
 is from east to west and from far to near.

 \textbf{Galaxy 1104 and Galaxy 1407} have at least
 3 times more H{\sc{I}} than predicted (see Fig. 7).
 Galaxy 1104 is a warped edge-on galaxy with a high warp amplitude. The
 H{\sc{I}} distribution is also rather asymmetric, suggesting a recent interaction.
 Galaxy 1407 is a star-forming galaxy with a large amount of H{\sc{I}} offset from the regularly rotating disk.
 It seems to be interacting with two close companions.

 \textbf{Galaxy 1378} has  less H{\sc{I}} gas than predicted and its H{\sc{I}} gas is highly
 lopsided.
 It is an isolated galaxy with strong on-going star formation at the center.
 This galaxy possesses a large amount of gas outside the regularly
 rotating disk, suggesting ram-pressure stripping or tidal stripping of H{\sc{I}}
 from the galaxy.

For comparison, we also present a set of ``non-outlier'' galaxies in Fig. 11. These are selected
randomly from our sample galaxies with both the offset to H{\sc I} mass-size relation and the offset
 to H{\sc I}-plane less than 0.2 dex. Generally speaking, the H{\sc I} shapes of these non-outliers are
more regular compared to the H{\sc I} shapes of outliers. Most of them are less asymmetric and have less
H{\sc I}-gas clouds in their outer region, which suggests no violent interaction with IGM.
The comparison between Fig. 10 and Fig. 11 confirms that most of the outliers really have very
irregular H{\sc I} morphologies.

Fig. 12 compares $\Delta$Center (left panel) and $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$
(right panel) between outliers and non-outliers.
Note that the non-outlier sample includes all the non-outliers defined in the
same way as above, not only those shown in Fig. 11.
The outliers appear to have larger $\Delta$Center and smaller $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$
 when compared to the non-outliers. This result is
consistent with the conclusion above, which are drawn from the example H{\sc I} maps
in Fig. 11. However, given the small sample size and the resulting poor statistics indicated by
 the K-S tests (see the K-S probabilities quoted in the figure),
this result should not be overemphasized.
 We list $\Delta$Center and $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ for the outliers
 in table 2. Galaxy 1700 has very large
$\Delta$Center ($\sim$0.9) that is consistent with its clearly biased H{\sc I} distribution.
Galaxy 1407 and Galaxy 983 have relatively large $\Delta$Center ($\sim$0.5),
which are attributed to their extra-planar gas.
Galaxy 1104, Galaxy 1554 and Galaxy 1407 have the largest $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$ among others.
Their location on H{\sc I}-plane are all above the mean relation. This is consistent with what we find in Fig. 9.
However, we don't compare $rs$ and $rs/R1$ for the outliers, as their $rs$
cannot be well determined.

\section{Summary and discussion}
In this paper, we present a catalogue of galaxies from the Bluedisk H{\sc{I}} galaxy survey that
includes sources within the cubes that were not specifically targeted for observation.
These galaxies are nevertheless very interesting, because they probe the environments
of unusually H{\sc I}-rich galaxies, as well as a control sample of galaxies with similar
masses and structural properties, but with more normal H{\sc I} content.

We present the distribution of H{\sc{I}} morphological parameters, the H{\sc I} mass-size relation and
scaling relations between H{\sc I} gas mass fraction and galaxy mass, structure and colour.
The main results in this work are listed below.
\begin{itemize}
\item Our sample follows established  H{\sc{I}} scaling relations as
function of stellar mass, stellar surface density and colour very well, and fits  the
 H{\sc{I}} mass-size relation, except for a few outliers.
\item  Galaxies in the H{\sc I}-rich cubes are displaced to higher H{\sc I} gas mass fractions than predicted
by the optical properties, compared to galaxies in the control cubes.
\item We inspect the H{\sc{I}} intensity maps and velocity fields of the outliers from the H{\sc{I}} mass-size
relation and the  plane.
 We find that all these galaxies are likely to have undergone recent
interaction  with their environment.
\end{itemize}

The phenomenon of  galactic conformity was first discovered  by \cite{Weinmann-06}, who argued that
the properties of satellite galaxies are strongly correlated with those of  their central
galaxies. In particular,  early-type central galaxies have  a larger fraction of
early-type satellites than late-type central galaxies with the same stellar mass.
Subsequently, \cite{Kauffmann-Li-Heckman-10} found that the total mass of gas in satellites
has a strong correlation with the colours and specific star formation
rates of central galaxies of
all stellar masses, and that this correlation extends out to
radii of 1  Mpc or more. This suggests that more gas-rich galaxies
should have more gas in satellites in their immediate surroundings.
This work was, however, based on optical proxies for H{\sc I} content and not on real H{\sc I} data.
In this paper, we find that galaxies in the large-scale environment of H{\sc{I}}-rich targeted galaxies
tend to be H{\sc{I}}-rich and to have a larger $R_{\rm 90,H{\sc I}}/R_{\rm 50,H{\sc I}}$.
Our findings thus support the conjectures presented in \citep{Kauffmann-Li-Heckman-10}.

\citet{Weinmann-06} and \citet{Ann-Park-Choi-08} argued that the X-ray-emitting hot gas of
host early-type central galaxies can deprive their satellites of their gas reservoirs
through hydrodynamic interactions. However, this cannot explain the conformity
effect in low mass halos. \citet{Kauffmann-Li-Heckman-10} argued that satellite galaxies
trace the high density peaks of underlying reservoir of ionized gas, which provides
fuel for star formation in central galaxies.

In this work  we have been able to study a few  galaxies which have irregular H{\sc{I}} shapes and
anomalous  H{\sc{I}} gas content. In most cases, we find signatures of interaction with the environment
that is suggestive of tidal or ram pressure stripping,
though two galaxies are found (1407 and 1104) that
may be  accreting  H{\sc{I}} clouds.

\section*{Acknowledgments}

EW and CL would like to thank the hospitality of the Max Planck
Institute for Astrophysics while this work was being initiated.
EW is grateful to Paolo Serra and Zhixiong Liang for helpful discussion on
data analysis progress, to Milan den Heijer for providing
the Gauss-Hermite velocity maps, and to Attila Popping
for readily providing his primary beam attenuation model.
This work is supported by National Key Basic Research Program
of China (No. 2015CB857004), NSFC (Grant No. 11173045, 11233005,
11325314, 11320101002), the Strategic Priority Research
Program ``The Emergence of Cosmological Structures'' of CAS
(Grant No. XDB09000000), and the exchange program between CAS
and the Max Panck Society.

Funding for  the SDSS and SDSS-II  has been provided by  the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, the  U.S.  Department of Energy,  the National Aeronautics
and Space Administration, the  Japanese Monbukagakusho, the Max Planck
Society,  and the Higher  Education Funding  Council for  England. The
SDSS Web  Site is  http://www.sdss.org/.  The SDSS  is managed  by the
Astrophysical    Research    Consortium    for    the    Participating
Institutions. The  Participating Institutions are  the American Museum
of  Natural History,  Astrophysical Institute  Potsdam,  University of
Basel,  University  of  Cambridge,  Case Western  Reserve  University,
University of Chicago, Drexel  University, Fermilab, the Institute for
Advanced   Study,  the  Japan   Participation  Group,   Johns  Hopkins
University, the  Joint Institute  for Nuclear Astrophysics,  the Kavli
Institute  for   Particle  Astrophysics  and   Cosmology,  the  Korean
Scientist Group, the Chinese  Academy of Sciences (LAMOST), Los Alamos
National  Laboratory, the  Max-Planck-Institute for  Astronomy (MPIA),
the  Max-Planck-Institute  for Astrophysics  (MPA),  New Mexico  State
University,   Ohio  State   University,   University  of   Pittsburgh,
University  of  Portsmouth, Princeton  University,  the United  States
Naval Observatory, and the University of Washington.

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